Listing of Contents to TAP Magazine Online #1 Tap 1.01 Intro to Tap Online Tap 1.02 Subscription to Tap Magazine Information Tap 1.03 Department of Defense Network Tap 1.04 TAC Access Control System by Argonaut Tap 1.05 Department of Defense Host Listing Tap 1.06 Letters to Tap Magazine Tap 1.07 Hacking Answering Machines by Predat0r Tap 1.08 NASA Space Shuttle Press Kit Tap 1.09 Ringback in the 502 NPA by Predat0r Tap 1.10 Tymcard Challenge by Techno-Cowboy Tap 1.11 Abbreviation List by Predat0r Tap 1.12 California Bbs Listing Tap 1.13 Nynex by Nightcrawler Tap 1.14 Red Phone Bbs Buffer Tap 1.15 Guide to school lockers by Cablecast Operator & Silver Sphere Tap 1.16 How to contact TAP via the WWIVnet with Wwivnet listing Welcome to the first issue of TAP Magazine Online. Publishing an electronic newsletter is somewhat easier then the hardcopy TAP, but i think i can continue to do this with some regularity, while still publishing TAP Magazine. It feels i am jumping on the band wagon since now days it seems everyone is publishing their own newsletter just to be famous or well known. I salute the true pioneers who have stuck it out and to those who have been inspirations to us all. The freedom of information shall never die as long as a few dedicated people continue to fight for our given rights. I have no set format yet, and don't plan on making anything fancy. I have just collected a few text files and thrown them together for those out there to read. If you want to get something included in TAP you can send it to me. If you want to get TAP Online issues first call the following boards. Blitzkrieg 502-499-8933 home to TAP and myself. Amerika's Most Wanted Bbs 502-491-2749 Hall of Injustice 502-241-9304 All these systems have been up for at least six months and are 24 hours. I would like to have other boards in different area codes distribute for me also, so if you want to do this contact me. I would now like to greet my fellow friends whom i have met in the computer underground. If i leave anyone out i am sorry. The Last Mafioso & The West Coast Phone Phreaks of Anarchist Express. Where the hell did you all disappear to? Iron Feather Journal, Phantasy, Phrack, Computer Underground Digest, Activist Times Inc and Ground Zero & TCC Crew, Network Information Access, and any other group which sends their files to my bbs regularly. Greets goto Aristotle who helped restart TAP then decided he wanted out. So now what are you going to do write for 2600? I hope not, sellout! and now sit back and enjoy the show..... Predat0r / Editor & Publisher of TAP Magazine. Subscription Information ============ =========== $10.00 for 10 issues USA rate. $15.00 for 10 issues in Canada. $20.00 for 10 issues Overseas. TAP Magazine will take CASH, Money Orders, Checks, or Postal Money Orders. Send to the following: TAP Magazine Post Office Box 20264 Louisville, Kentucky 40250-0264 Predat0r / Editor & Publisher of TAP Magazine. Subscription Information ============ =========== $10.00 for 10 issues USA rate. $15.00 for 10 issues in Canada. $20.00 for 10 issues Overseas. TAP Magazine will take CASH, Money Orders, Checks, or Postal Money Orders. Send to the following: TAP Magazine Post Office Box 20264 Louisville, Kentucky 40250-0264 Greetings fellow CyberNauts: This gem was downloaded from the DDN on the InterNet. It is a good guide for learning to hack the Net. If you like what you see leave note for Argonaut at Rivendell BBS (816) 563-4845. This is my Home of Port and a small but growing hack/phreak node. The Argonaut =========================================================================== FEATURES OF THE TAC ACCESS CONTROL SYSTEM (TACACS) To log in to the network via a MILNET TAC, you MUST have a unique ID and Access Code (TAC Access Card). These cards are issued by the DDN Network Information Center (NIC) only after a user has been authorized by the Host Administrator of the host on which the user has his primary mailbox or account. IF YOU HAVE NOT RECEIVED YOUR TAC ACCESS CARD, AND HAVE A LEGITIMATE REQUIREMENT TO ACCESS THE NETWORK VIA A MILNET TAC, CONTACT YOUR HOST ADMINISTRATOR! (DO NOT CONTACT THE NIC FOR AUTHORIZATION). If you do not know who your Host Administrator is, you may find out by using the "WHOIS" command on the NIC.DDN.MIL host. Instructions on using "WHOIS" are as follows: When you finish reading this message, type "quit" as instructed. After the connection to NIC.DDN.MIL is closed, type "@n" again. You will be told how to find your Host Administrator. When finished, type "logout" at the prompt and you will be returned to the TAC. ---------------------------------------------------------------------- TACACS, the access control system for MILNET TACs, requires you to log in before a connection to a host may be completed. The login process is automatically started with the first @open (@o) command you issue. There is a @close (@c) command to close the TAC connection and also a @logout (@l) command to logout. Otherwise, the functioning of the TAC is essentially unaffected by the access control system. Here is a sample of the login dialogue: First, the command to get the TAC's attention is Control-Q. (a) PVC-TAC 111 #: 01 This is the last line of the TAC herald, which the TAC uses to identify itself. When you see the herald, the TAC is ready for your command. (b) @o 26.2.0.8 The user inputs the command to ------------------- open a connection plus the internet address of the host to which he wishes to connect, followed by a Carriage Return. (c) TAC Userid: SAMPLE.LOGIN Here the TAC prompts the user for -------------------- his Userid. The user enters his ID exactly as shown as shown on his TAC Access Card, followed by a Carriage Return. (d) Access Code: 22bgx4467 Again the TAC prompts the user, ----------------- who responds by entering his Access Code as shown on his TAC Access Card, followed by a Carriage Return. (e) Login OK The TAC validates the ID/Access TCP trying...Open code and proceeds to open the requested connection. HELPFUL INFORMATION: When entering your TAC Userid and Access Code: - A carriage return terminates each input line and causes the next prompt to appear. - As you type in your TAC Userid and Access Code, it does not matter whether you enter an alphabetic character in upper or lower case. All lower case alphabetic characters echo as upper case for the Userid. - The Access Code is not echoed in full-duplex mode. An effort is made to obscure the Access Code printed on hardcopy terminals in half-duplex mode. - You may edit what you type in by using the backspace (Control-H) key to delete a single character. - You may delete the entire line and restart by typing Control-U. A new prompt will appear. - While entering either the TAC Userid or Access Code, you may type Control-C to abort the login process and return to the TAC command mode. You must interrupt or complete the login process in order to issue any TAC command. - The @reset (@r) command resets the TAC and returns you to the TAC welcome banner. IF YOU HAVE A PROBLEM WITH TAC LOGIN: Should the login sequence fail (as indicated by the response "Bad login"), examine your Access Card carefully to ensure that you are entering the ID and Access Code correctly. Note that Access Codes never contain a zero, a one, a "Q" or a "Z", as each of these characters may be mistaken for another character. If you see what appears to be one of these characters in your access code, it is really the letter "O" (oh), or "G" (gee), the letter "L" (el), or the number "2" (two). If you have followed all of the above steps as indicated, and if you are sure you are entering your ID and Access Code correctly, and you still cannot log in, call the Network Information Center at (415) 859-3695 or (800) 235-3155 for help. AFTER LOGGING IN: Your TAC port will remain logged in as long as you have an open connection. If you close the connection, you will have ten minutes in which to reopen a connection without having to log in again. If you do not reopen a connection within ten minutes, the TAC will attempt to hang up your port, and will automatically log you out. WHEN YOU ARE FINISHED: Always close the connection using "@c" then log out using the "@l" command. Typing "@r" (reset) has no effect on your logged-in status. If you now wish to log in to the TAC, leave the TACNEWS program by typing "quit" at the next prompt. This will return you to the TAC, and you may then begin the login sequence with the @o command to the TAC. Another InterNet gem from the treasure chest of the Argonaut For more InterNet info call: RIVENDELL BBS: (816) 563-4845 # DoD Internet Host Table InterNet node address 6.1.0.1 yuma-emh1.army.mil yuma.arpa yuma1.army.mil 7.8.0.2 protolaba.dca.mil protolaba.arpa 7.0.0.3 edn-vax.dca.mil edn-vax.arpa 8.0.0.2 ccs.bbn.com 8.1.0.2 cci.bbn.com bbncci.arpa 8.3.0.2 ccd.bbn.com bbnccd.arpa 8.5.0.2 cck.bbn.com 8.0.0.5 cd2.bbn.com 8.2.0.5 cc1-tac.bbn.com 8.3.0.9 bbnnet2-arpanet-gw.arpa bbnnet2-arpanet-gw.bbn.com 8.7.0.9 egonoc.bbn.com 8.0.0.10 cc4-tac.bbn.com 8.3.0.10 jsnach.bbn.com jsnach.arpa 8.1.0.12 noc3.bbn.com 8.5.0.14 dev.cs.net 128.89.0.94 dev.cs.net 8.1.0.16 rvax.bbn.com 128.89.0.132 rvax.bbn.com 8.1.0.18 cc2.bbn.com 8.7.0.18 cca.bbn.com bbncca.arpa 8.6.0.19 cc3-tac.bbn.com 8.9.0.19 ccny.bbn.com 8.2.0.24 ccu.bbn.com bbnccu.arpa 8.3.0.24 cco.bbn.com 8.0.0.26 ccp.bbn.com 8.1.0.26 ccq.bbn.com bbnccq.arpa 8.3.0.26 hnoc.bbn.com 8.5.0.26 z.bbn.com bbnz.arpa 8.7.0.26 ccx.bbn.com bbnccx.arpa 8.8.0.26 ccy.bbn.com bbnccy.arpa 8.16.0.33 cce.bbn.com bbncce.arpa 8.1.0.35 col.bbn.com bbncc-columbia.arpa 8.2.0.37 cc-vm.bbn.com 8.0.0.58 idnoc.bbn.com 8.0.0.97 noc4.bbn.com 10.4.0.5 gw-1.cs.net 192.31.103.1 gw-1.cs.net 192.5.58.1 gw-1.cs.net 10.7.0.5 lpr-netman.arpa lpr-netman.bbn.com 10.2.0.7 rand-arpa-tac.arpa 10.2.0.11 su-arpa-tac.arpa 10.3.1.11 stanford.arpa 10.5.0.14 white.incsys.com incremental.arpa 192.31.230.1 white.incsys.com incremental.arpa 10.6.0.14 cadre.dsl.pitt.edu cadre.arpa cadre.dsl.pittsburgh.edu 128.147.128.1 cadre.dsl.pitt.edu cadre.arpa cadre.dsl.pittsburgh.edu 128.147.1.1 cadre.dsl.pitt.edu cadre.arpa cadre.dsl.pittsburgh.edu 130.49.128.1 cadre.dsl.pitt.edu cadre.arpa cadre.dsl.pittsburgh.edu 10.8.0.14 gateway.sei.cmu.edu 128.237.254.254 gateway.sei.cmu.edu 128.2.237.251 gateway.sei.cmu.edu 10.4.0.17 tis.com tis.arpa 10.2.0.20 dcec-arpa-tac.arpa 10.3.0.20 edn-unix.dca.mil edn-unix.arpa 10.5.0.20 dcec-psat.arpa 10.11.0.20 sccgate.scc.com sccgate.arpa 10.1.21.27 mcon.isi.edu 10.0.21.22 mcon.isi.edu 10.1.22.27 speech11.isi.edu 10.1.23.27 wbc11.isi.edu isi-wbc11.arpa 10.0.23.22 wbc11.isi.edu isi-wbc11.arpa 10.1.89.27 setting.isi.edu isi-setting.arpa 10.1.91.27 pallas-athene.isi.edu isi-pallas-athene.arpa 10.1.97.27 aikane.isi.edu isi-aikane.arpa 10.1.98.27 czar.isi.edu isi-czar.arpa 10.1.99.27 mycroft.isi.edu isi-mycroftxxx.arpa 10.1.124.27 cmr.isi.edu isi-cmr.arpa 10.1.156.27 png11.isi.edu 10.1.254.27 echo.isi.edu isi-echo.arpa 10.0.0.28 arpa3-tac.arpa 10.1.0.31 amc.xait.xerox.com cca-vms.arpa 10.4.0.31 xait-arp-tac.arpa cca-arp-tac.arpa 10.0.0.46 collins-pr.arpa 10.1.0.46 collins-gw.arpa 192.12.172.11 collins-gw.arpa 10.7.0.51 a-lhi-sri-03.arpa 10.3.1.54 jpl-robotics.arpa 10.1.0.63 bbn-arpa-tac.arpa 10.2.0.77 mit-arpa-tac.arpa 10.3.0.77 umass-gw.cs.umass.edu unix1.cs.umass.edu 128.119.40.12 umass-gw.cs.umass.edu unix1.cs.umass.edu 10.0.0.82 tacac.arpa 10.1.0.82 a-lhi-bbn-01.arpa 10.5.0.82 arpa-mc.arpa arpanet-mc.arpa 10.5.0.96 prc-gw.prc.unisys.com 10.2.0.99 vax-x25.arpa 10.3.0.99 bbn-x25-test3.arpa 10.4.0.99 bbn-x25-test4.arpa 10.5.0.99 test-host5-x25.arpa 10.0.0.115 anoc1.arpa 10.0.0.126 tycho.ncsc.mil tycho.arpa 10.1.0.126 afterlife.ncsc.mil afterlife.arpa 13.2.16.8 parcvax.xerox.com vaxc.xerox.com 13.1.100.206 arisia.xerox.com 13.0.12.232 xerox.com xerox.arpa 14.0.0.4 vtest.cs.ucl.ac.uk ucl-vtest.arpa 14.0.0.5 ess-tun.cs.ucl.ac.uk 14.0.0.9 tunnel.cs.ucl.ac.uk 15.255.152.2 sde.hp.com 15.255.16.7 hplabs.hp.com hplabs.arpa 16.1.0.1 decwrl.dec.com wrl.dec.com 16.10.0.1 vixie.sf.ca.us 16.1.0.2 gatekeeper.dec.com 16.1.0.3 cerberus.pa.dec.com 16.1.0.8 src.dec.com decsrc.dec.com 16.1.0.9 wsl.dec.com 18.72.2.1 mit.edu 18.77.0.2 mitlns.mit.edu 18.85.0.2 media-lab.media.mit.edu 18.87.0.2 euler.mit.edu 18.92.0.2 coventry.mit.edu 18.72.0.3 bitsy.mit.edu 18.79.0.3 lids.mit.edu 18.85.0.3 atrp.media.mit.edu 18.87.0.3 cauchy.mit.edu 18.92.0.3 mitvma.mit.edu 18.71.0.4 orpheus.mit.edu 18.86.0.4 xv.mit.edu 18.87.0.4 abel.mit.edu 18.79.0.5 lmpvax.mit.edu 18.86.0.5 dolphin.mit.edu 18.87.0.5 stokes.mit.edu 18.10.0.6 sludge.lcs.mit.edu mit-sludge.arpa 18.26.0.134 sludge.lcs.mit.edu mit-sludge.arpa 128.127.25.101 sludge.lcs.mit.edu mit-sludge.arpa 18.62.0.6 eddie.mit.edu mit-eddie.mit.edu 18.72.0.6 priam.mit.edu 18.85.0.6 ems.media.mit.edu 18.86.0.6 sloan.mit.edu 18.87.0.6 banach.mit.edu 18.71.0.7 jason.mit.edu 18.87.0.7 fermat.mit.edu 18.72.0.8 achilles.mit.edu 18.87.0.8 bourbaki.mit.edu math.mit.edu 18.10.0.9 gross.ai.mit.edu mit-gross.arpa 128.52.22.9 gross.ai.mit.edu mit-gross.arpa 128.52.14.1 gross.ai.mit.edu mit-gross.arpa 128.52.32.1 gross.ai.mit.edu mit-gross.arpa 18.87.0.9 archimedes.mit.edu 18.75.0.10 space.mit.edu 18.87.0.10 fourier.mit.edu 18.87.0.11 newton.mit.edu 18.71.0.12 paris.mit.edu 18.87.0.12 noether.mit.edu 18.80.0.13 charon.mit.edu 18.87.0.13 zermelo.mit.edu 18.72.1.14 eagle.mit.edu 18.80.0.14 prometheus.mit.edu 18.87.0.14 borel.mit.edu 18.87.0.15 poisson.mit.edu 18.87.0.16 schubert.mit.edu 18.62.0.17 dspvax.mit.edu mit-bugs-bunny.arpa 18.80.0.17 bloom-beacon.mit.edu 18.87.0.17 boole.mit.edu 18.27.0.18 fft.mit.edu 18.87.0.18 galois.mit.edu 18.27.0.19 dft.mit.edu 18.87.0.19 laplace.mit.edu 18.27.0.20 porky.mit.edu 18.87.0.20 ramanujan.mit.edu 18.92.0.20 po.mit.edu 18.27.0.21 sam.mit.edu 18.87.0.21 turing.mit.edu 18.87.0.22 russell.mit.edu 18.87.0.23 hypatia.mit.edu emma.mit.edu 18.87.0.24 laurent.mit.edu 18.87.0.25 bessel.mit.edu 18.87.0.26 cantor.mit.edu 18.87.0.27 fibonacci.mit.edu 18.87.0.28 lebesgue.mit.edu 18.87.0.29 pythagoras.mit.edu 18.85.0.30 hq.media.mit.edu 18.87.0.30 von-neumann.mit.edu 18.87.0.31 polya.mit.edu 18.87.0.32 pascal.mit.edu 18.87.0.33 euclid.mit.edu 18.87.0.34 bernoulli.mit.edu 18.30.0.35 cls.lcs.mit.edu mit-cls.arpa 18.87.0.35 hausdorff.mit.edu 18.26.0.36 xx.lcs.mit.edu lcs.mit.edu mit-xx.arpa 18.87.0.36 dedekind.mit.edu 18.87.0.37 jacobi.mit.edu 18.71.0.38 prep.ai.mit.edu 18.87.0.38 hermite.mit.edu 18.72.0.39 athena.mit.edu mit-athena.arpa 18.87.0.39 tarski.mit.edu 18.87.0.40 markov.mit.edu 18.87.0.41 godel.mit.edu goedel.mit.edu 18.88.0.55 cogito.mit.edu 18.27.0.56 goldilocks.lcs.mit.edu mit-goldilocks.arpa 18.10.0.71 pm-prj.lcs.mit.edu mit-prj.arpa 18.26.0.80 melange.lcs.mit.edu grape-nehi.lcs.mit.edu 18.88.0.80 hstbme.mit.edu 18.88.0.82 infoods.mit.edu 18.88.0.85 psyche.mit.edu 18.52.0.92 theory.lcs.mit.edu mit-theory.arpa 18.88.0.92 erl.mit.edu 18.26.0.94 thyme.lcs.mit.edu jhereg.lcs.mit.edu toadkiller-dog.lcs.mit.edu 18.26.0.95 larch.lcs.mit.edu mit-larch.arpa 18.26.0.98 rinso.lcs.mit.edu mit-rinso.arpa 18.26.0.106 tide.lcs.mit.edu mit-tide.arpa mit-tide tide 18.26.0.107 dash.lcs.mit.edu mit-dash.arpa mit-dash dash 18.26.0.114 hq.lcs.mit.edu 18.82.0.114 mgm.mit.edu 18.26.0.115 allspice.lcs.mit.edu ptt.lcs.mit.edu 18.26.0.121 lithium.lcs.mit.edu 18.72.0.122 ra.mit.edu 18.72.0.142 arktouros.mit.edu 18.71.0.151 mit-strawb.arpa strawb.mit.edu 18.70.0.160 w20ns.mit.edu 18.26.0.176 zurich.ai.mit.edu 18.80.0.181 osborn.mit.edu 18.80.0.191 delphi.mit.edu 18.30.0.192 vx.lcs.mit.edu mit-vax.arpa mit-vx.arpa mit-vax.lcs.mit.edu 18.10.0.195 big-blue.lcs.mit.edu mit-big-blue.arpa 18.48.0.195 live-oak.lcs.mit.edu oak.lcs.mit.edu 18.72.0.205 garp.mit.edu 18.30.0.206 zermatt.lcs.mit.edu 18.30.0.212 expo.lcs.mit.edu 18.48.0.216 wild-blue-yonder.lcs.mit.edu wild-blue.lcs.mit.edu 18.86.0.216 diamond.mit.edu 18.62.0.232 caf.mit.edu mit-caf.arpa 26.1.0.1 oberursel.mt.ddn.mil oberursel-mil-tac.arpa 26.3.0.1 rhe-eds.af.mil rhe-eds.arpa 26.5.0.1 obl-ignet.army.mil obe-ignet.arpa 26.6.0.1 pcc-obersl.army.mil 26.7.0.1 oberursel-emh1.army.mil email-oberursl.army.mil 26.0.0.2 emmc.dca.mil eur-milnet-mc.arpa 26.1.0.2 patch.mt.ddn.mil minet-vhn-mil-tac.arpa 26.3.0.2 eur.dca.mil dca-eur.arpa dca-eur.dca.mil 26.4.0.2 moehringen-emh1.army.mil 26.5.0.2 moehringen-ignet.army.mil igmirs-moehringer.arpa 26.6.0.2 patch.dca.mil patch.arpa 26.8.0.2 goeppingen-emh1.army.mil email-goeppngn.army.mil 26.9.0.2 nellingen-emh1.army.mil email-nellingn.army.mil 26.10.0.2 pcc-moeh.arpa moeh-pcc.army.mil 26.11.0.2 pcc-nell.arpa nel-pcc.army.mil 26.12.0.2 pcc-boeb.arpa bbl-pcc.army.mil 26.13.0.2 pcc-vaih.arpa vhn-pcc.army.mil 26.14.0.2 patch2.mt.ddn.mil vaihingen2-mil-tac.arpa 26.15.0.2 frg.bbn.com bbncc-eur.arpa 26.16.0.2 erf-boe.arpa bbl-erf.army.mil 26.0.0.3 sandiego.mt.ddn.mil sandiego-tac.arpa 26.1.0.3 trout.nosc.mil nosc.mil trout.nosc.navy.mil 128.49.16.7 trout.nosc.mil nosc.mil trout.nosc.navy.mil 26.2.0.3 logicon.arpa 26.3.0.3 nprdc.navy.mil nprdc.arpa nprdc.mil 192.5.65.1 nprdc.navy.mil nprdc.arpa nprdc.mil 26.4.0.3 mcdn-cpt.arpa 26.5.0.3 sdcsvax.ucsd.edu 128.54.20.1 sdcsvax.ucsd.edu 26.6.0.3 navelex.arpa 26.7.0.3 navelexnet-sd.arpa 26.8.0.3 sds-sandgoa.arpa sds-sandgoa.navy.mil 26.9.0.3 mirnas.arpa 26.11.0.3 navmeducapendleton.arpa 26.12.0.3 sssd.arpa 26.13.0.3 navmeducasandiego.arpa 26.14.0.3 sandiego-httds.arpa 26.15.0.3 scubed.com scubed.arpa scubed.scubed.com 192.31.63.10 scubed.com scubed.arpa scubed.scubed.com 192.16.16.70 scubed.com scubed.arpa scubed.scubed.com 26.16.0.3 grunion.nosc.mil nosc-ether.arpagrunion.nosc.navy.mil 192.42.2.2 grunion.nosc.mil nosc-ether.arpagrunion.nosc.navy.mil 26.18.0.3 comnavsurfpac.arpa 26.0.0.4 zwe-eds.af.mil zwe-eds.arpa 26.1.0.4 campbell-bks.mt.ddn.mil campbllbks-mil-tac.arpa 26.2.0.4 heidelberg-emh1.army.mil heidelberg-emh.arpa 26.4.0.4 heidelberg-perddims.army.mil perddims-hei.arpa 26.5.0.4 edas-scw.arpa szn-edasscw.army.mil 26.6.0.4 cpo-man-eur.arpa mhn-cpo.army.mil 26.7.0.4 hdg-ignet1.army.mil hhsp-ignet.arpa 26.8.0.4 hdg-ignet2.army.mil hei2-ignet.arpa 26.9.0.4 jacs6333.army.mil 26.14.0.4 pcc1.arpa hdg-pcc.army.mil 26.15.0.4 ccpd.arpa hdg-ccpd.army.mil 26.16.0.4 cpo-hdl-eur.arpa hdg-cpo.army.mil 26.1.0.5 karl-shurz.mt.ddn.mil bremerhaven-mil-tac.arpa 26.4.0.5 pals-68.arpa brn-pals1.army.mil 26.5.0.5 pals-67.arpa brn-pals.army.mil 26.6.0.5 oldendorf-am1.af.mil 26.7.0.5 bremrhvn-meprs.army.mil 26.8.0.5 bremerhave-emh1.army.mil email-klshzksn.army.mil 26.10.0.5 bremerhave-asims.army.mil brm-asims.arpa 26.11.0.5 dasps-e-562-b.arpa obl-daspseb.army.mil 26.12.0.5 gst-ignet.army.mil gar-ignet.arpa 26.13.0.5 mtmc-aif-b.arpa brn-aifb.army.mil 26.0.0.6 rotterdam.mt.ddn.mil minet-rdm-mil-tac.arpa 26.5.0.6 sostrbrg-piv.af.mil 26.6.0.6 cna-eds.af.mil cna-eds.arpa 26.7.0.6 schinnen-emh1.army.mil 26.9.0.6 rotterdam-emh1.army.mil email-rotterdm.army.mil 26.10.0.6 mtmc-aif.arpa rotterdam-aif.army.mil 26.11.0.6 dasps-e-778.arpa rotterdam-daspse.army.mil 26.13.0.6 mtf-sosbg.af.mil mtf-sosbg.arpa mtf-cp-newamsterdam.arpa 26.1.0.7 london.mt.ddn.mil minet-lon-mil-tac.arpa 26.4.0.7 ben-eds.af.mil ben-eds.arpa 26.6.0.7 chievres-emh1.army.mil 26.10.0.7 alc-eds.af.mil alc-eds.arpa 26.11.0.7 kem-eds.af.mil kem-eds.arpa 26.12.0.7 london-ncpds.arpa 26.0.0.8 washdc-nrl.mt.ddn.mil nrlwashdc-mil-tac.arpa 26.3.0.8 ccf.nrl.navy.mil ccf3.nrl.navy.mil nrl.arpa nrl3.arpa 128.60.0.3 ccf.nrl.navy.mil ccf3.nrl.navy.mil nrl.arpa nrl3.arpa 26.5.0.8 nardacwash-001.arpa 26.7.0.8 spawar-003.arpa 26.8.0.8 sds-cda1.arpa sds-cda1.navy.mil 26.9.0.8 navelexnet-ward.arpa 26.10.0.8 ships-donoacs.arpa 26.11.0.8 wnyosi2.arpa 26.11.2.8 wnysamis.arpa 26.11.3.8 wnyosi4.arpa 26.11.4.8 wnyosi7.arpa 26.13.0.8 amdahl-5850-vm.navy.mil 26.15.0.8 amdahl-v7a.navy.mil 26.16.0.8 amdahl-v7.navy.mil 26.17.0.8 ibm4381.navy.mil 26.20.0.8 nfe.nrl.navy.mil nrl-nfe.arpa 128.60.1.1 nfe.nrl.navy.mil nrl-nfe.arpa 192.26.26.1 nfe.nrl.navy.mil nrl-nfe.arpa 26.21.0.8 arctan.nrl.navy.mil nrl-arctan.arpa 26.1.0.9 sigonella.mt.ddn.mil sigonella-mil-tac.arpa 26.3.0.9 com-eds.af.mil com-eds.arpa 26.4.0.9 san-eds.af.mil san-eds.arpa 26.6.0.9 sig-ncpds.arpa 26.7.0.9 mtf-comiso.af.mil 26.8.0.9 comiso-am1.af.mil comiso-am1.arpa 26.10.0.9 comiso-piv.af.mil 26.1.0.10 rota.mt.ddn.mil rota-mil-tac.arpa 26.2.0.10 mtf-rota.arpa mtf-rota.af.mil 26.6.0.10 rota-ncpds.arpa 26.0.0.11 corona.mt.ddn.mil corona-mil-tac.arpa 26.4.0.11 fltac-poe.arpa 26.6.0.11 santaana-dmins.dla.mil 26.7.0.11 c.navy.mil dgoa.arpa 26.8.0.11 fltac-sperry.arpa 26.9.0.11 norton-ro1.af.mil norton-ro1.arpa 26.10.0.11 afsc-bsd.af.mil afsc-bmo.af.mil afsc-bmo.arpa 26.12.0.11 norton-piv-2.af.mil norton-piv-2.arpa 26.13.0.11 afisc-01.af.mil afisc-01.arpa 26.15.0.11 corona-po.arpa 192.31.174.2 corona-po.arpa 26.0.0.12 vicenza.mt.ddn.mil vicenza-mil-tac.arpa 26.4.0.12 vca-asims.arpa vic-asims.army.mil 26.5.0.12 cpo-vic-eur.arpa vic-cpo.army.mil 26.6.0.12 afrts-vic.arpa vic-afrts.army.mil 26.7.0.12 vic-ignet.army.mil vic-ignet.arpa 26.8.0.12 emed-vicenza.arpa vic-emed.army.mil 26.9.0.12 meprs-vicenza.arpa vic-meprs.army.mil 26.10.0.12 jacs6335.arpa vic-hacs.army.mil 26.11.0.12 pcc-vice.arpa vic-pcc.army.mil 26.12.0.12 vicenza-emh1.army.mil email-vicenza.army.mil 26.0.0.13 gunter.mt.ddn.mil gunter-mil-tac.arpa 26.1.0.13 gunter-adam.af.mil gunter-adam.arpa 26.5.0.13 gunterp4.af.mil gunterp4.arpa 131.2.16.1 gunterp4.af.mil gunterp4.arpa 26.6.0.13 rucker-perddims.army.mil perddims06.arpa 26.7.0.13 bcgunt.af.mil bcgunt.arpa 26.11.0.13 jackson-perddims.army.mil perddims07.arpa 26.12.0.13 hrc-iris.af.mil hrc-iris.arpa 129.141.11.1 hrc-iris.af.mil hrc-iris.arpa 26.13.0.13 mtf-gunter.af.mil mtf-gunter.arpa 26.14.0.13 gu-eds.af.mil gu-eds.arpa 26.15.0.13 camnet-maxwell-r01.af.mil camnet-maxwell-r01.arpa 26.18.0.13 maxwell-am1.af.mil maxwell-am1.arpa camnet-maxw-r03.arpa 26.5.0.14 zweibrucke-asims.army.mil asims-zweibrucken.arpa 26.8.0.14 dmaoe.dma.mil dmaodsdoe.arpa 26.13.0.14 cpo-prm-eur.arpa pms-cpo.army.mil 26.14.0.14 cpo-zwi-eur.arpa zbn-cpo.army.mil 26.1.0.15 ramstein.mt.ddn.mil ramstein-mil-tac.arpa 26.5.0.15 van-eds.af.mil van-eds.arpa 26.8.0.15 camnettwo-ramstein.af.mil camnettwo-ramstein.arpa 26.9.0.15 camnet-ramstein.af.mil camnet-ramstein.arpa 26.16.0.15 erf-nah.arpa zbn-erfnah.army.mil 26.0.0.16 moffett.mt.ddn.mil moffett-mil-tac.arpa 26.1.0.16 arc-psn.arc.nasa.gov 26.2.0.16 amelia.nas.nasa.gov ames-nas.arpa ames-nas.nas.nasa.gov 129.99.20.1 amelia.nas.nasa.gov ames-nas.arpa ames-nas.nas.nasa.gov 26.3.0.16 nas-psn.nas.nasa.gov ames-nasb.arpa 10.1.0.8 nas-psn.nas.nasa.gov ames-nasb.arpa 128.102.32.5 nas-psn.nas.nasa.gov ames-nasb.arpa 26.4.0.16 mofnaf.navy.mil mofnaf.arpa 26.13.0.128 mofnaf.navy.mil mofnaf.arpa 26.6.0.16 sac-misc6.af.mil sac-misc6.arpa 26.8.0.16 gtewd.af.mil gtewd.arpa 26.0.0.17 mclean2.mt.ddn.mil mclean2-mil-tac.arpa 26.2.0.17 mclean.mt.ddn.mil mitre-mil-tac.arpa 26.3.0.17 mitre.arpa mwunix.mitre.org 128.29.104.0 mitre.arpa mwunix.mitre.org 26.6.0.17 his-fsd6.arpa 26.7.0.17 his-fsd8.arpa 26.10.0.17 ncpds-arlington.arpa 26.11.0.17 ddn-wms.arpa ddn-wms.dca.mil 26.12.0.17 fstc-chville.arpa 26.13.0.17 mclean-unisys.army.mil 26.14.0.17 cnrc.arpa 26.15.0.17 sysr-7cg.af.mil sysr-7cg.arpa sysr-7cg-ddn.arpa 26.16.0.17 dulles-ignet.army.mil ignet-prc.arpa 26.18.0.17 osi-2-gw.dca.mil 26.17.0.17 osi-2-gw.dca.mil 26.19.0.17 beast.ddn.mil 192.33.3.2 beast.ddn.mil 26.0.0.18 multics.radc.af.mil radc-multics.arpa 26.1.0.18 drum-perddims.army.mil perddims27.arpa 26.2.0.18 griffiss.mt.ddn.mil radc-mil-tac.arpa 26.5.0.18 lonex.radc.af.mil radc-lonex.arpa 26.8.0.18 lons.radc.af.mil 26.9.0.18 coins.cs.umass.edu cs-umass.edu 26.10.0.18 softvax.radc.af.mil radc-softvax.arpa 26.12.0.18 sutcase.af.mil sutcase.arpa 26.13.0.18 ftdrum-meprs.army.mil 26.14.0.18 griffiss-piv-1.af.mil 26.17.0.18 electra.cs.buffalo.edu buffalo-cs.arpa 128.205.34.9 electra.cs.buffalo.edu buffalo-cs.arpa 26.18.0.18 cs.rit.edu rit.arpa 26.24.0.18 mtf-plattsburgh.af.mil 26.27.0.18 ftdrum-ignet.army.mil 26.28.0.18 drum-tcaccis.army.mil 26.0.0.19 eagle.nist.gov nbs-vms.arpa nist.nbs.gov 26.3.0.20 oo1.af.mil oo1.arpa 26.4.0.20 hillmdss.af.mil hillmdss.arpa 26.5.0.20 hill.mt.ddn.mil hill1-mil-tac.arpa 26.6.0.20 hill-piv-1.af.mil 26.7.0.20 remis-oo.af.mil 26.8.0.20 edcars-oo.af.mil edcars-oo.arpa 26.9.0.20 dsacs10.arpa 26.10.0.20 oodis01.af.mil oodis01.arpa 192.12.100.3 oodis01.af.mil oodis01.arpa 26.11.0.20 aflc-oo-aisg1.af.mil aflc-oo-aisg1.arpa 26.12.0.20 mt-home-piv-1.af.mil mt-home-piv-1.arpa 26.13.0.20 mednet-oo.af.mil mednet-oo.arpa 26.16.0.20 ogden-dmins.dla.mil 26.19.0.20 snag-oo.af.mil snag-oo.arpa 26.4.0.21 sm-eds.af.mil sm-eds.arpa 26.5.0.21 oaknsc.navy.mil oaknsc.arpa 26.7.0.148 oaknsc.navy.mil oaknsc.arpa 26.7.0.21 oms-nws.navy.mil 26.0.0.22 mcclellan.mt.ddn.mil mcclellan-mil-tac.arpa 26.5.0.22 mcclelln-am1.af.mil mcclelln-am1.arpa 26.6.0.22 c3po.af.mil sm-alc-c3po.arpa 131.105.1.1 c3po.af.mil sm-alc-c3po.arpa 26.7.0.22 aflc-sm-dmmis1-si01.af.mil aflc-sm-dmmis1-si01.arpa 26.8.0.22 smdis01.af.mil rdb-sm.arpa 26.9.0.22 edcars-mcclellan.af.mil edcars-mcclellan.arpa 26.11.0.22 travis-piv-2.af.mil travis-piv-2.arpa 26.13.0.22 lewis-perddims.army.mil perddims20.arpa 26.18.0.22 beale-piv-1.af.mil 26.24.0.22 snag-sm.af.mil snag-sm.arpa 26.0.0.23 mcclellan2.mt.ddn.mil mcclellan2-mil-tac.arpa 26.4.0.23 sm1.af.mil sm1.arpa 26.5.0.23 mcclellan-mdss.af.mil mcclellan-mdss.arpa 26.6.0.23 aflc-sm-aisg1.af.mil aflc-sm-aisg1.arpa 26.8.0.23 netpmsa-bangor1.dca.mil netpmsa-bangor1.arpa terpss-ttf2.arpa 26.10.0.23 remis-sm.af.mil 26.12.0.23 mednet-sm.af.mil mednet-sm.arpa 26.0.0.24 nadc.arpa 26.1.0.24 dcrp.dla.mil dcrp.arpa 26.11.0.24 dcrp.dla.mil dcrp.arpa 26.3.0.24 johnsville.mt.ddn.mil johnsville-tac.arpa 26.5.0.24 ncpds-phili1.navy.mil ncpds-phili1.arpa 26.6.0.24 ncpds-phili2.navy.mil ncpds-phili2.arpa 26.7.0.24 dmadp.dma.mil dmaodsdcp.arpa 26.8.0.24 disc.arpa 26.9.0.24 dpsc.dla.mil dpsc.arpa 26.12.0.24 navmeducaphil.arpa 26.13.0.24 pera-crudes.navy.mil pera-crudes.arpa 26.14.0.24 burroughs-dev-2.dca.mil burroughs-dev-2.arpa 26.15.0.24 burroughs-dev-1.dca.mil burroughs-dev-1.arpa 26.19.0.24 philashpyd-poe.navy.mil philashpyd-poe.arpa 26.24.0.24 ccsu.arpa 26.2.0.25 mil-eds.af.mil mil-eds.arpa 26.3.0.25 croughton.mt.ddn.mil croughton-mil-tac.arpa 26.5.0.25 gre-eds.af.mil gre-eds.arpa 26.7.0.25 blnhmcsc-am1.af.mil 26.8.0.25 alconbry-piv-2.af.mil 26.9.0.25 mtf-upperheyford.af.mil mtf-upperheyford.arpa 26.11.0.25 upp-eds.af.mil upp-eds.arpa 26.12.0.25 fairford-am1.af.mil 26.14.0.25 mtf-ltlrsgtn.af.mil 26.15.0.25 mtf-fairford.af.mil mtf-fairford.arpa 26.16.0.25 mtf-grnhmcmn.af.mil 26.0.0.26 pentagon.mt.ddn.mil pentagon-mil-tac.arpa 26.1.0.26 pentagon-ignet.army.mil igmirs-daig.army.mil igmirs-daig.arpa 26.2.0.26 haflee.af.mil haflee.arpa 26.4.0.26 pentagon-opti.army.mil optimis-pent.arpa pentagon-emh1.army.mil 26.5.0.26 pent-gw-hq.af.mil 26.5.10.26 aad-hq.af.mil 26.5.27.26 hq.af.mil 26.5.70.26 vm7cg.af.mil vm7cg.arpa 26.6.0.26 msddnpent.af.mil msddnpent.arpa 26.7.0.26 coan.af.mil coan.arpa 26.8.0.26 fms2.af.mil fms2.arpa 26.12.0.26 navelexnet-crystal.arpa 26.13.0.26 nardac-nohims.arpa 26.24.0.26 opsnet-pentagon.af.mil opsnet-pentagon.arpa 26.1.0.27 holy-loch.mt.ddn.mil minet-hlh-mil-tac.arpa 26.4.0.27 oslo-am1.af.mil 26.6.0.27 menwithhill-am1.af.mil 26.8.0.27 dmris-keflavik.arpa 26.1.0.28 elmendorf.mt.ddn.mil elmendorf-mil-tac.arpa 26.2.0.28 ftrichardson-ignet.army.mil ignet-172d-infbde.arpa 26.4.0.28 richardson-perddims.army.mil perddims43.arpa 26.9.0.28 elmendrf-am1.af.mil elmendrf-am1.arpa 26.10.0.28 elmendorf-piv-2.af.mil elmendorf-piv-2.arpa 26.11.0.28 richards-tcaccis.army.mil 26.14.0.28 decco-ak.arpa 26.15.0.28 altos1.af.mil altos1.arpa 26.0.0.29 aberdeen.mt.ddn.mil brl-mil-tac.arpa 26.1.0.29 apg-emh1.apg.army.mil apg-1.apg.army.mil apg-1.arpa 26.2.0.29 brl.arpa brl.mil 26.4.0.29 dis.dla.mil dis.arpa 26.6.0.29 apg-emh2.army.mil apg-2.arpa 26.7.0.29 csta-1.apg.army.mil csta-one.arpa 26.9.0.29 apg-perddims.army.mil perddims38.arpa 26.14.0.29 aberdeen-ignet2.army.mil 26.20.0.29 apg-emh3.apg.army.mil apg-3.apg.army.mil apg-3.arpa 26.21.0.29 apg-emh4.apg.army.mil apg-4.apg.army.mil apg-4.arpa 26.22.0.29 apg-emh7.army.mil ilcn-apg.arpa 26.0.0.30 brooks.mt.ddn.mil brooks-mil-tac.arpa 26.1.0.30 afmpc-2.af.mil afmpc-2.arpa 26.2.0.30 sam-housto-mil80.army.mil mil-80-5bde.arpa 26.11.0.30 tisg-6.af.mil tisg-6.arpa 26.12.0.30 hqhsd.brooks.af.mil bafb-ddnvax.arpa 26.13.0.30 ed-san-ant.af.mil ed-san-ant.arpa 26.4.0.31 sds-norflka.arpa sds-norflka.navy.mil 26.6.0.31 monroe-tdss.army.mil 26.7.0.31 netpmsa-norfolk1.dca.mil netpmsa-norfolk1.arpa 26.8.0.31 nardacva.arpa 26.9.0.31 pera-asc.arpa 26.10.0.31 idanf.arpa 26.11.0.31 spawar08.arpa 26.12.0.31 seacenlant-portsmth.navy.mil 26.13.0.31 nohimsmidlant.arpa 26.14.0.31 qedvb.arpa 26.16.0.31 navmeducacda.arpa 26.17.0.31 cinclant-norfolk.navy.mil 26.18.0.31 ftmonroe-ignet2.army.mil monroe-ignet2.army.mil 26.24.0.31 norndc.navy.mil norndc.arpa 26.25.0.31 comnavairlant.navy.mil 26.26.0.31 sub-force.navy.mil 26.27.0.31 subship-portsmouth.navy.mil 26.0.0.32 greeley.mt.ddn.mil greely-mil-tac.arpa 26.5.0.32 ftgreely-adacs.army.mil 26.2.0.33 monterey.mt.ddn.mil nps-mil-tac.arpa 26.5.0.33 monterey-perddims.army.mil perddims36.arpa 26.6.0.33 cs.nps.navy.mil nps-cs.arpa 131.120.1.10 cs.nps.navy.mil nps-cs.arpa 26.7.0.33 monterey-asbn.army.mil 26.20.0.33 cc.nps.navy.mil nps.arpa 26.0.0.34 lbl-gw.arpa 26.4.0.34 san-franci-mil80.army.mil mil-80-6bde.arpa 26.6.0.34 mare-island-shipyd.navy.mil 26.10.0.34 vallejo1.arpa 26.11.0.34 netpmsa-vallej01.arpa terpss-vallej01.arpa 26.12.0.34 netpmsa-vallejo2.arpa terpss-vallejo2.arpa 26.13.0.34 netpmsa-vallejo3.arpa 26.0.0.35 sandiego2.mt.ddn.mil san-diego-mil-tac.arpa 26.1.0.35 nosc-tecr.arpa tecr.arpa tecr.nosc.mil 26.2.0.35 nosc-secure2.arpa 26.3.0.35 nosc-secure3.arpa 26.5.0.35 ntsc-pac.arpa vaxpac.arpa 26.6.0.35 nardac-sandiego.arpa 26.8.0.35 netpmsa-sandiego1.arpa 26.9.0.35 netpmsa-sandiego2.navy.mil 26.10.0.35 moccw.navy.mil 26.11.0.35 sndndc.arpa 26.12.0.35 sndndc.arpa 26.14.0.35 corona-pad4.arpa 26.15.0.35 nuwes-sd.navy.mil 26.16.0.35 bendix-sd.arpa 26.18.0.35 seacenpac-sandiego.navy.mil 26.1.0.36 hawaii-emh.pacom.mil hawaii-emh.arpa 26.3.0.36 smith.mt.ddn.mil hawaii2-mil-tac.arpa 26.5.0.36 nstcpvax.arpa ieln-ntecph.arpa 26.6.0.36 honolulu.army.mil perddims45.arpa 26.11.0.36 netpmsa-pearl1.arpa 26.1.0.37 atlanta-asims.army.mil asims-rdca1.arpa 26.2.0.37 mcpherson.mt.ddn.mil mcpherson-mil-tac.arpa 26.3.0.37 ftgillem-darms2.army.mil gillem-darms.army.mil 26.5.0.37 mcpherson-darms2.army.mil darms-2.arpa 26.6.0.37 mcpherson-darms1.army.mil darms-1.arpa 26.7.0.37 gordon-perddims.army.mil perddims32.arpa 26.9.0.37 columbia-aim1.af.mil columbia-aim1.arpa 26.11.0.37 soraaa.army.mil soraaa.arpa 26.13.0.37 gordon-jacs6360.army.mil gordon-jacs.army.mil 26.14.0.37 shaw-piv-1.af.mil shaw-piv-1.arpa 26.0.0.38 great-lakes.mt.ddn.mil greatlakes-mil-tac.arpa 26.5.0.38 dlsc1.arpa 26.14.0.115 dlsc1.arpa 26.6.0.38 drms.arpa comtenc.arpa 26.6.0.115 drms.arpa comtenc.arpa 26.7.0.38 dlsc2.arpa 26.7.0.115 dlsc2.arpa 26.9.0.38 netpmsa-gtlakes1.arpa 26.10.0.38 netpmsa-gtlakes2.arpa 26.11.0.38 netpmsa-gtlakes3.arpa 26.13.0.38 kisawyer-am1.af.mil kisawyer-am1.arpa 26.14.0.38 sheridan-asims2.army.mil 26.15.0.38 kisawyer-piv-1.af.mil kisawyer-piv-1.arpa 26.16.0.38 navmeducaglakes.arpa 26.29.0.38 sds-glakesa.arpa sds-glakesa.navy.mil 26.0.0.39 edwards.mt.ddn.mil edwards-mil-tac.arpa 26.1.0.39 edwards-2060.af.mil edwards-2060.arpa 26.2.0.39 edwards-vax.af.mil edwards-vax.arpa 26.6.0.39 mtf-edwards.af.mil mtf-edwards.arpa 26.7.0.39 george-piv-1.af.mil george-piv-1.arpa 26.8.0.39 norton-piv-1.af.mil norton-piv-1.arpa 26.9.0.39 edwards-piv-1.af.mil edwards-piv-1.arpa 26.11.0.39 edwards-am1.af.mil edwards-am1.arpa 26.13.0.39 edwards-argus.af.mil edwards-argus.arpa 26.14.0.39 asims-047.arpa 26.15.0.39 edwards-saftd-2.af.mil 26.0.0.40 cambridge.mt.ddn.mil bbn-mil-tac.arpa 26.3.0.40 ccz.bbn.com 26.4.0.40 supship-boston.navy.mil supship-boston.arpa 26.8.0.40 plattsburgh-piv-1.af.mil plattsburgh-piv-1.arpa 26.9.0.40 gw1.hanscom.af.mil esdvax2.arpa 129.53.0.101 gw1.hanscom.af.mil esdvax2.arpa 26.10.0.40 navmedcl-portsmouth.arpa 26.11.0.40 westover-piv-1.af.mil westover-piv-1.arpa 26.14.0.40 pease-piv-1.af.mil 26.16.0.40 ftdevens-meprs.army.mil 26.17.0.40 boston-dmins.dla.mil 26.29.0.40 nocws.dca.mil 26.0.0.41 redstone.mt.ddn.mil redstone-mil-tac.arpa 26.1.0.41 redstone-emh3.army.mil micom-test.arpa 26.2.0.41 redstone-emh4.army.mil usarec-2.arpa 26.3.0.41 milneth.ornl.gov ornl-msr.arpa 26.4.0.41 campbell-perddims.army.mil perddims14.arpa 26.5.0.41 bdmsc-hunt.arpa 26.6.0.41 redstone-perddims.army.mil perddims30.arpa 26.7.0.41 netpmsa-milln1.arpa 26.8.0.41 ncpds-oakridge9.arpa 26.9.0.41 redstone-ato.arpa 26.10.0.41 ncpds-oakridge8.arpa 26.11.0.41 mtf-montgomery.af.mil mtf-montgomery.arpa 26.8.0.79 mtf-montgomery.af.mil mtf-montgomery.arpa 26.12.0.41 idamfs.arpa 26.13.0.41 columbus-aim1.af.mil columbus-aim1.arpa 26.14.0.41 aedc-vax.af.mil 26.15.0.41 dsreds.arpa 26.16.0.41 camnet-arnold-r01.af.mil camnet-arnold-r01.arpa 26.17.0.41 redstone-meprs.army.mil 26.24.0.41 redstone-ignet.army.mil 26.25.0.41 redstone-emh2.army.mil micom.arpa 26.14.0.209 redstone-emh2.army.mil micom.arpa 26.26.0.41 redstone-emh1.army.mil mic01.arpa 26.7.0.209 redstone-emh1.army.mil mic01.arpa 26.0.0.42 ramstein2.mt.ddn.mil ramstein2-mil-tac.arpa 26.3.0.42 ramstein2-emh.af.mil ramstein2-emh.arpa ram-emc.arpa 26.7.0.42 ram-esims.af.mil ram-esims.arpa 26.8.0.42 ramstein-piv-1.af.mil ramstein-piv-1.arpa 26.9.0.42 lrc-eds.af.mil lrc-eds.arpa 26.10.0.42 ram-eds.af.mil ram-eds.arpa 26.11.0.42 baumholder-emh1.army.mil email-baumholdr.army.mil 26.12.0.42 mtf-ramstein.arpa mtf-ramstein.af.mil 26.14.0.42 mtf-hq.af.mil mtf-hq.arpa 26.15.0.42 ald-gdss.af.mil 26.15.0.15 ald-gdss.af.mil 26.0.0.43 shafter.mt.ddn.mil shaftr-mil-tac.arpa 26.4.0.43 shafter-asims.army.mil asims-045.arpa 26.5.0.43 pod-har.army.mil 26.6.0.43 pepo41.army.mil 26.7.0.43 deers-asmo.navy.mil 26.8.0.43 hawaii-emh1.pacom.mil 26.9.0.43 ftshafter-ignet2.army.mil 26.10.0.43 pod-hon.army.mil 26.8.0.100 pod-hon.army.mil 26.13.0.43 ftshaftr-jacs6358.army.mil 26.16.0.43 tamc-meprs.army.mil 26.18.0.43 pep042.army.mil 26.0.0.44 navmeducaorlando.arpa 26.1.0.44 ntsc-ate.arpa 26.3.0.44 orlando.mt.ddn.mil orlando-mil-tac.arpa 26.4.0.44 orlando-httds.arpa 26.6.0.44 sperry-system-11.dca.mil sperry-system-11.arpa sperry11.arpa 26.9.0.44 ftlauderdale.nswc.navy.mil nswc-fl.arpa 26.10.0.44 sds-orlanda.navy.mil 26.14.0.44 netpmsa-orlan4.arpa 26.15.0.44 netpmsa-orlan4.arpa 26.16.0.44 ntsc-74.navy.mil ntsc-74.arpa 26.17.0.44 ntsc-sef.arpa 26.18.0.44 orlando-emh1.army.mil pmtrade.arpa 26.0.0.45 dovernj.mt.ddn.mil ardec-mil-tac.arpa 26.1.0.45 pica.army.mil ardec.arpa 26.2.0.45 bayonne-tcaccis.army.mil tcaccis-bay.arpa 26.3.0.45 dover-emh1.army.mil pica-qa.arpa qa.pica.army.mil 26.6.0.45 dcrn2.arpa 26.10.0.58 dcrn2.arpa 26.11.0.45 pltsbrgh-am1.af.mil pltsbrgh-am1.arpa 26.13.0.45 drum-asims.army.mil asims-006.arpa 26.17.0.45 gw.pica.army.mil pica.arpa 192.12.8.4 gw.pica.army.mil pica.arpa 129.139.1.4 gw.pica.army.mil pica.arpa 26.20.0.45 dover-emh2.army.mil pica-lca.arpa lca.pica.army.mil 26.2.0.46 port-hueneme.mt.ddn.mil porthueneme-mil-tac.arpa 26.4.0.46 ptmpmt.arpa 26.5.0.46 dsacs08.army.mil dsacs08.arpa 26.6.0.46 navmeducahueneme.arpa 26.17.0.46 vaxb.navy.mil nswses.arpa vaxb.nswses.navy.mil 192.31.106.3 vaxb.navy.mil nswses.arpa vaxb.nswses.navy.mil 26.0.0.47 wrightpat.mt.ddn.mil wpafb-mil-tac.arpa 26.1.0.47 wpafb-afwal.arpa 26.2.0.47 wpafb-jalcf.arpa wpafb-jalcf.af.mil 26.6.0.47 dsac-g1.arpa 26.7.0.47 wpafb-afwp1.af.mil wpafb-afwp1.arpa 26.8.0.47 wright-pat-piv-1.af.mil 26.9.0.47 amis.af.mil amis.arpa 26.12.0.47 c-17igp.af.mil c-17igp.arpa 26.14.0.47 extender.afit.af.mil afitnet.arpa 26.15.0.47 logair-gw.arpa 192.31.226.1 logair-gw.arpa 26.18.0.47 wpafb-info5.af.mil wpafb-info5.arpa wpafb-info1.af.mil 26.21.0.47 wpafb-fdl.af.mil wpafb-fdl.arpa 26.22.0.47 lognet2.af.mil lognet2.arpa 192.12.64.2 lognet2.af.mil lognet2.arpa 26.0.0.48 kirtland.mt.ddn.mil kirtland-mil-tac.arpa 26.2.0.48 ddnvx2.afwl.af.mil afwl-vax.arpa 129.238.32.36 ddnvx2.afwl.af.mil afwl-vax.arpa 26.4.0.48 dna-field-command.dca.mil dna-field-command.arpa 26.5.0.48 ddnvx1.afwl.af.mil afwl.arpa 129.238.32.2 ddnvx1.afwl.af.mil afwl.arpa 26.6.0.48 dna-cafrms.arpa 26.7.0.48 kirtland-piv-rjets.af.mil kirtland-piv-rjets.arpa 26.9.0.48 hqafosp.af.mil hqafosp.arpa 26.11.0.48 afotec2.af.mil afotec2.arpa 26.14.0.48 cannon-piv-1.af.mil cannon-piv-1.arpa 26.0.0.49 ddn3.dca.mil ddn3.arpa 26.5.0.49 ncpds-argentia.arpa 26.6.0.49 devens-emh1.army.mil usaisd-aims.arpa 26.9.0.49 mtf-pease.af.mil mtf-pease.arpa 26.11.0.49 devens-asims.army.mil asims-022.arpa 26.12.0.49 loring-piv-1.af.mil loring-piv-1.arpa 26.14.0.49 submept.navy.mil submepp.arpa 26.0.0.50 alexandria.mt.ddn.mil darcom-mil-tac.arpa 26.1.0.50 alexandria-emh2.army.mil ari-hq1.arpa 26.2.0.50 alexandria-emh1.army.mil amc-hq.arpa 26.3.0.50 alexandria-emh3.army.mil pyramid-amc.arpa 26.4.0.50 alexandria-mil80.army.mil mil-80-per1.arpa 26.5.0.50 cafrms.arpa 26.6.0.50 washington-asims.army.mil asims-rdcw1.arpa 26.7.0.50 asims-dpcb1.arpa 26.10.0.50 moc120.arpa 26.11.0.50 radmis-onr.arpa 26.14.0.50 fmpmis.navy.mil 26.20.0.50 alexandria-emh4.army.mil usadhq2.arpa 26.21.0.50 etl.army.mil etl.arpa 26.22.0.50 alexandria-emh5.army.mil amc-4.arpa 26.0.0.51 randolph2.mt.ddn.mil randolph2-mil-tac.arpa 26.4.0.51 randolph-piv-1.af.mil randolph-piv-1.arpa 26.6.0.51 san-antonio-piv-2.af.mil 26.7.0.51 afmpc1.af.mil afmpc1.arpa 26.8.0.51 afmpc3.af.mil afmpc3.arpa 26.10.0.51 mtf-kelly.af.mil mtf-kelly.arpa 26.11.0.51 ddp1.af.mil ddp1.arpa 26.13.0.51 randolph-piv-3.af.mil randolph-piv-3.arpa 26.0.0.52 randolph3.mt.ddn.mil randolph3-mil-tac.arpa 26.4.0.52 camnet-randolph-r01.af.mil camnet-randolph-r01.arpa 26.5.0.52 sam-housto-darms.army.mil darms-7.arpa 26.8.0.52 san-antonio-piv-1.af.mil san-antonio-piv-1.arpa 26.11.0.52 randolph2-pc3.af.mil randolph2-pc3.arpa 26.12.0.52 mtf-bergstrom.af.mil mtf-bergstrom.arpa 26.15.0.52 afmpc-10.af.mil afmpc-10.arpa 26.16.0.52 randolph-pc3.af.mil randolph-pc3.arpa 26.17.0.52 bergstrm-am1.af.mil bergstrm-am1.arpa 26.0.0.53 uv6.eglin.af.mil afsc-ad.arpa 26.3.0.53 eglin.mt.ddn.mil afsc-ad-mil-tac.arpa 26.5.0.53 tyndall-am1.af.mil 26.6.0.53 uv4.eglin.af.mil eglin-vax.arpa 26.9.0.53 ntsc-pen.arpa 26.10.0.53 netpmsa-pens1.arpa 26.13.0.53 penndc.navy.mil penndc.arpa 26.5.0.158 penndc.navy.mil penndc.arpa 26.14.0.53 hrlbrtfd-am1.af.mil hrlbrtfd-am1.arpa camnet-hurl-r01.arpa 26.15.0.53 camnet-hurl-r02.af.mil camnet-hurl-r02.arpa 26.16.0.53 eglin-am1.af.mil eglin-am1.arpa 26.18.0.53 wims-tyn1.af.mil wims-tyn1.arpa 26.0.0.54 detrick.mt.ddn.mil detrick-mil-tac.arpa 26.1.0.54 ilcn-detrick.arpa 26.2.0.54 ritchie-perddims.army.mil perddims34.arpa 26.5.0.54 detrick-emh1.army.mil 26.6.0.54 detrick-hsc.army.mil hsc-detrick1.arpa 26.7.0.54 letterkenn-emh1.army.mil lead-1.arpa 26.11.0.54 detrick-hsc2.army.mil hsc-detrick2.arpa 26.13.0.54 mipca.navy.mil pad.arpa 26.14.0.54 alexandria-onet.army.mil absalex-emh.army.mil abs-alex.arpa 26.3.0.55 sheridan-mil801.army.mil mil-80-sher1.arpa 26.4.0.55 sheridan-mil802.army.mil mil-80-sher56.arpa 26.7.0.55 sperblomn.dca.mil sperblomn.arpa 26.10.0.55 dcri.arpa 26.8.0.38 dcri.arpa 26.11.0.55 xenurus.gould.com 26.13.0.55 crane-emh1.army.mil caaa.arpa 26.14.0.55 indinpls.navy.mil 26.16.0.55 wurtsmith-piv-1.af.mil wurtsmith-piv-1.arpa 26.29.0.55 mcs.anl.gov anl-mcs.arpa 26.0.0.57 dockmaster.ncsc.mil dockmaster.dca.mil dockmaster.arpa 26.4.0.58 hanscom-piv-1.af.mil hanscom-piv-1.arpa 26.8.0.58 wva-emh1.army.mil wva-1.arpa 26.15.0.58 supshipbrooklyn.arpa 26.0.0.59 scott.mt.ddn.mil scott-mil-tac.arpa 26.6.0.59 macisin-ii.af.mil macisin-ii.arpa 26.13.0.59 hqmac-gdss.af.mil hqmac-gdss.arpa 26.14.0.59 macisin-i.af.mil macisin-i.arpa 26.15.0.59 acfp-dev.af.mil 26.0.0.60 monmouth.mt.ddn.mil monmouth-mil-tac.arpa 26.1.0.60 cecom-2.arpa monmouth-emh2.army.mil 26.7.0.60 monmouth-perddims.army.mil perddims28.arpa 26.8.0.60 dix-perddims.army.mil perddims26.arpa 26.9.0.60 ftmonmth-meprs.army.mil 26.10.0.60 bayonne-autostrad.army.mil autostrad-bay.arpa 26.14.0.58 bayonne-autostrad.army.mil autostrad-bay.arpa 26.14.0.60 navwepstaearle.arpa 26.15.0.60 mcguire-piv-2.af.mil mcguire-piv-2.arpa 26.16.0.60 dover-piv-2.af.mil dover-piv-2.arpa 26.17.0.60 monmouth-emh1.army.mil networks.arpa 26.24.0.60 cecom-3.arpa monmouth-emh3.army.mil 26.0.0.61 saint-louis.mt.ddn.mil stlouis-mil-tac.arpa 26.3.0.61 st-louis-emh3.army.mil avscom.arpa 26.5.0.61 dmaac.dma.mil dmaacgad.arpa 26.7.0.61 st-louis-avnmam.army.mil dasp75.arpa 26.9.0.61 stlouis-ignet.army.mil st-louis-ignet.army.mil 26.10.0.61 whiteman-piv-1.af.mil whiteman-piv-1.arpa 26.15.0.61 stlouis-ignet2.army.mil st-louis-ignet2.army.mil 26.16.0.61 simastl.army.mil 192.35.148.1 simastl.army.mil 26.19.0.61 st-louis-emh4.army.mil stl4.arpa 26.0.0.62 roberts.mt.ddn.mil roberts-mil-tac.arpa 26.2.0.62 navmeducalemoore.arpa 26.6.0.62 vandenberg-am1.af.mil vandenberg-am1.arpa 26.8.0.62 lemnaf.navy.mil lemnaf.arpa 26.6.0.135 lemnaf.navy.mil lemnaf.arpa 26.17.0.62 roberts-emh1.army.mil 26.0.0.63 el-segundo2.mt.ddn.mil elsegundo-mil-tac.arpa 26.4.0.63 afsc-sdx.af.mil afsc-sdx.arpa 26.5.0.63 navmeducalongbeach.arpa 26.6.0.63 dava1.af.mil dava1.arpa 26.7.0.63 lbnsy.arpa 192.41.202.2 lbnsy.arpa 26.9.0.63 jpl-gdss.af.mil jpl-gdss.arpa 26.10.0.63 la-pacdpinet.army.mil 26.11.0.63 mtf-mather.af.mil 26.12.0.63 navshipyd-longbeach.arpa 26.13.0.63 supship-long-beach.arpa 26.15.0.63 van-nuys-dmins.dla.mil 26.16.0.63 elsegundo-dmins.dla.mil 26.24.0.63 losalmts-darms.army.mil 26.0.0.64 robins.mt.ddn.mil robins-mil-tac.arpa 26.4.0.64 ftmcpherson-ignet.army.mil forscom-ignet.army.mil igmirs-forscom .arpa 26.8.0.64 gillem-mil80.army.mil mil-80-2bde.arpa 26.9.0.64 wr-hits.af.mil wr-hits.arpa 26.10.0.64 snag-wr.af.mil snag-wr.arpa 26.12.0.64 ftgillm-ignet.army.mil igmirs-ftgillm.army.mil igmirs-ftgillm.ar pa 26.13.0.64 robinsmdss.af.mil robinsmdss.arpa 26.16.0.64 robins-piv-1.af.mil 26.0.0.65 el-segundo.mt.ddn.mil elsegundo2-mil-tac.arpa 26.2.0.65 aerospace.aero.org aero.org 192.5.9.3 aerospace.aero.org aero.org 130.221.192.10 aerospace.aero.org aero.org 26.4.0.65 jpl-milvax.arpa 128.1.13.0 jpl-milvax.arpa 26.11.0.65 dcrl.dla.mil dcrl.arpa 26.14.0.230 dcrl.dla.mil dcrl.arpa 26.30.0.65 afsc-ssd.af.mil afsc-sd.af.mil 26.1.0.66 afgl.arpa 26.2.0.66 hanscom.mt.ddn.mil afgl-mil-tac.arpa 26.6.0.66 eastlonex.radc.af.mil radc-eastlonex.arpa 26.7.0.66 gtewis.af.mil gtewis.arpa 26.8.0.66 gw2.hanscom.af.mil esdvax.arpa 26.13.0.66 afgl-vax.af.mil afgl-vax.arpa 26.14.0.66 drcvax.af.mil drcvax.arpa 26.15.0.66 hanscom-am1.af.mil hanscom-am1.arpa 26.19.0.66 supship-bath.navy.mil supship-bath.arpa 26.0.0.67 andrews.mt.ddn.mil afsc-hq-mil-tac.arpa 26.1.0.67 afsc-hq.arpa afsc-hq.af.mil 26.2.0.67 hqafsc-vax.af.mil hqafsc-vax.arpa 26.7.0.67 mqg.dca.mil mqg.arpa 26.9.0.67 indianhead.nswc.navy.mil nswc-ih.arpa 26.10.0.67 ftmeade-darms.army.mil meade-darms.army.mil darms-4.arpa 26.11.0.67 navsea-331.navy.mil 26.12.0.67 alexandria-ignet1.army.mil igmirs-cidc.army.mil igmirs-cidc.arpa 26.14.0.67 hqafsc-lons.af.mil 26.15.0.67 alexandria-ignet.army.mil igmirs-darcom.arpa 26.16.0.67 navsea-pms313.navy.mil 26.17.0.67 andrews-piv-1.af.mil andrews-piv-1.arpa 26.0.0.69 abrams2.mt.ddn.mil abrams2-mil-tac.arpa 26.4.0.69 frankfurt-asims.army.mil fra-asims.arpa 26.7.0.69 hanau-emh1.army.mil email-hanau.army.mil 26.8.0.69 aschaffenb-emh1.army.mil 26.10.0.69 frankfurt-ignet2.army.mil fra-ignet.army.mil 26.12.0.69 dar-ignet.army.mil 26.14.0.69 euraaa.army.mil 26.0.0.70 cmsc.dca.mil cmsc.arpa 26.3.0.70 dcaoc2.mt.ddn.mil dcaoc2-mil-tac.arpa 26.6.0.70 washngtn-meprs.army.mil 26.7.0.70 anacostia-onet.navy.mil 26.8.0.70 navyyard-onet.navy.mil 26.19.0.70 ddntrouble.dca.mil ddntrouble.arpa 26.0.0.71 okc-unix.arpa 26.1.0.71 ftsill-ignet.army.mil sill-ignet.army.mil igmirs-sill-ig.arpa 26.2.0.71 tinker.mt.ddn.mil tinker-mil-tac.arpa 26.3.0.71 satods.arpa 26.4.0.71 tinkermdss.af.mil tinkermdss.arpa 26.6.0.71 ccso-vax.af.mil ccso-vax.arpa 131.18.3.1 ccso-vax.af.mil ccso-vax.arpa 26.10.0.71 oc1.af.mil oc1.arpa 26.12.0.71 ocdis01.af.mil 26.14.0.71 aflc-oc-aisg1.af.mil 26.16.0.71 apsd-ii-os062.af.mil apsd-ii-os062.arpa 26.17.0.71 tinker-piv-1.af.mil tinker-piv-1.arpa 26.24.0.71 chaffe-tcaccis.army.mil 26.0.0.72 ddn-shadow-mc.dca.mil ddn-shadow-mc.arpa 26.1.0.72 ilcn-natick.arpa 26.2.0.72 ddn2.dca.mil ddn.dca.mil ddn2.arpa ddn.arpa 26.5.0.72 inmet.inmet.com inmet.com ddnt.arpa 26.6.0.72 devens-perddims.army.mil perddims19.arpa 26.7.0.72 watertown-emh1.army.mil 26.8.0.72 x25test.dca.mil x25test.arpa 26.9.0.72 dcrb2.arpa 26.7.0.58 dcrb2.arpa 26.11.0.72 nsyptsmh-poe.arpa nsyportsmouth.arpa nysportsmouth.arpa 192.26.20.2 nsyptsmh-poe.arpa nsyportsmouth.arpa nysportsmouth.arpa 26.12.0.72 loring-am1.af.mil loring-am1.arpa 26.14.0.72 pease-am1.af.mil pease-am1.arpa 26.15.0.72 natick-emh1.army.mil natick1.arpa 26.0.0.73 sri-nic.arpa nic.ddn.mil 10.0.0.51 sri-nic.arpa nic.ddn.mil 26.3.0.73 menlo-park.mt.ddn.mil sri-mil-tac.arpa 26.5.0.73 twg.com twg.arpa 26.0.0.74 white-sands.mt.ddn.mil whitesands-mil-tac.arpa 26.2.0.74 wsmr-simtel20.army.mil simtel20.arpa simtel20.army.mil 26.4.0.74 ftbliss-ignet.army.mil bliss-ignet.army.mil igmirs-ftbliss.arpa 26.6.0.74 holloman-am1.af.mil holloman-am1.arpa 26.8.0.74 bliss-perddims.army.mil perddims02.arpa 26.11.0.74 wsmr-emh99.army.mil traps-wsmr.arpa 26.13.0.74 bliss-ato.army.mil bliss-ato.arpa 26.0.0.75 yuma.mt.ddn.mil yuma-mil-tac.arpa 26.5.0.75 luke-piv-3.af.mil luke-piv-3.arpa 26.8.0.75 nellis-piv-1.af.mil nellis-piv-1.arpa 26.10.0.75 mtf-nellis.af.mil mtf-nellis.arpa 26.1.0.76 dca-ems.dca.mil dca-ems.arpa dcems.arpa 26.3.0.76 dcaoc.mt.ddn.mil dcaoc-mil-tac.arpa 26.4.0.76 deers-alexandria.arpa 26.5.0.76 oahost.dca.mil oahost.arpa 26.6.0.76 belvoir-ignet2.army.mil igmirs-corpeng.arpa 26.10.0.76 pentagon-bcn.army.mil pentagon-bcn.arpa 192.31.75.235 pentagon-bcn.army.mil pentagon-bcn.arpa 26.17.0.76 conus-milnetmc.dca.mil conus-milnetmc.arpa 26.0.0.76 conus-milnetmc.dca.mil conus-milnetmc.arpa 26.2.0.77 zama.mt.ddn.mil zama-mil-tac.arpa 26.4.0.77 zama-ignet.army.mil ignet-cpzama.arpa 26.6.0.77 yokota-piv-1.af.mil yokota-piv-1.arpa 26.7.0.77 misawa-piv-1.af.mil misawa-piv-1.arpa 26.11.0.77 zama-pacdpine.army.mil pacdpinet-zama.arpa 26.13.0.77 mtf-misawa.arpa mtf-misawa.af.mil 26.14.0.77 ncpds-iwakuni.arpa 26.15.0.77 nsdyok.arpa yoknsd.arpa 26.10.0.77 nsdyok.arpa yoknsd.arpa 26.16.0.77 ida-fms-yokosuka.arpa 26.17.0.77 poj-har.army.mil poj-har.arpa 26.18.0.77 zama-emh1.army.mil 26.19.0.77 cpzama-jacs6350.army.mil 26.1.0.78 puget-sound.mt.ddn.mil pugetsound-mil-tac.arpa 26.5.0.78 peracv.navy.mil peracv.arpa 26.6.0.78 navhospbrem.arpa 26.7.0.78 navmeducabremerton.arpa 26.8.0.78 navmeducaoakharbor.arpa 26.15.0.78 lewis-asims.army.mil asims-020.arpa 26.0.0.79 benning.mt.ddn.mil benning-mil-tac.arpa 26.4.0.79 benning-ato.arpa 26.6.0.79 benning.army.mil 26.7.0.79 benning-tcaccis.army.mil 26.10.0.79 mcdn-alb.arpa 26.11.0.79 mtf-maxwell.af.mil mtf-maxwell.arpa 26.13.0.79 benning-jacs5074.army.mil jacs5074.arpa 26.14.0.79 columbus-am1.af.mil columbus-am1.arpa 26.15.0.79 camnet-columbus-r02.af.mil camnet-columbus-r02.arpa 26.16.0.79 gunter-am1.af.mil gunter-am1.arpa camnet-gunt-r01.arpa 26.18.0.79 benning-perddims.army.mil perddims33.arpa 26.19.0.79 benning-meprs.army.mil 26.24.0.79 ftgillem-darms.army.mil 26.25.0.79 ftmcphsn-jacs5073.army.mil 26.31.0.79 benning-asims.army.mil asims-034.arpa 26.0.0.80 bragg.mt.ddn.mil bragg-mil-tac.arpa 26.4.0.80 tecnet-clemson.arpa tecnet-clemson.jcte.jcs.mil 26.5.0.80 nardac-cherrypt.arpa 26.6.0.80 chrnsc.arpa 26.9.0.80 chrnsc.arpa 26.7.0.80 ed-mb.af.mil ed-mb.arpa 26.8.0.80 netpmsa-charl3.arpa 26.10.0.80 ftbragg-asatms.army.mil bragg-asatms.army.mil 26.11.0.80 navmeducacharleston.arpa 26.12.0.80 mcdn-clb3.arpa 26.13.0.80 bragg-asims.army.mil 26.14.0.80 jackson-jacs5056.army.mil jackson-jacs.army.mil 26.15.0.80 cptmas.arpa 26.16.0.80 navmeducalejeune.arpa 26.17.0.80 navmeducacherrypt.arpa 26.18.0.80 bragg-jacs5072.army.mil bragg-jacs.army.mil 26.19.0.80 ftbragg-ignet.army.mil bragg-ignet.army.mil 26.24.0.80 pope-piv-1.af.mil pope-piv-1.arpa 26.25.0.80 ftbragg-ignet2.army.mil bragg-ignet2.army.mil 26.26.0.80 ftbragg-ignet3.army.mil bragg-ignet3.army.mil 26.30.0.80 bragg-emh1.army.mil bragg.arpa 26.31.0.80 bragg-perddims.army.mil perddims10.arpa 26.0.0.81 carderock.mt.ddn.mil david-mil-tac.arpa 26.3.0.81 dtrc.dt.navy.mil dtrc.arpa 130.46.1.3 dtrc.dt.navy.mil dtrc.arpa 26.6.0.81 dmacsc.dma.mil dmaodshost.arpa 26.9.0.81 hqaaa.army.mil hqaaa.arpa 26.11.0.81 nardacdc002.arpa dcmail.arpa 26.20.0.81 wrair-emh1.army.mil ilcn-wreed.arpa wrair.arpa 26.2.0.82 buckner.mt.ddn.mil buckner-mil-tac.arpa 26.5.0.82 navmeducaokinawa.arpa 26.6.0.82 ncpds-butler.arpa 26.7.0.82 kadena-piv-1.af.mil kadena-piv-1.arpa 26.8.0.82 kadena-c01.af.mil kadena-c01.arpa 26.9.0.82 kadena-c02.af.mil kadena-c02.arpa 26.10.0.82 mtf-kadena.af.mil mtf-kadena.arpa 26.12.0.82 kadena-am2.af.mil kadena-am2.arpa 26.13.0.82 sac-misc3.af.mil sac-misc3.arpa 26.18.0.82 buckner-emh1.army.mil 26.0.0.83 robins2.mt.ddn.mil robins2-mil-tac.arpa 26.5.0.83 wr1.af.mil wr1.arpa 26.6.0.83 wrdis01.af.mil 26.7.0.83 edcars-wr.af.mil edcars-wr.arpa 26.8.0.83 aflc-wr-aisg1.af.mil aflc-wr-aisg1.arpa 26.9.0.83 dmmis-wr.af.mil dmmis-wr.arpa 26.10.0.83 robins-am1.af.mil robins-am1.arpa 26.11.0.83 kngtrf.navy.mil kngtrf.arpa 26.15.0.205 kngtrf.navy.mil kngtrf.arpa 26.12.0.83 moody-am1.af.mil moody-am1.arpa 26.13.0.83 robins-piv-2.af.mil 26.15.0.83 robins-pc3.af.mil robins-pc3.arpa 26.16.0.83 remis-wr.af.mil 26.2.0.84 dahlgren.mt.ddn.mil nswc-mil-tac.arpa 26.3.0.84 oas.nswc.navy.mil nswc-oas.arpa Letters to TAP Magazine TAP Magazine Issue #101 December 1st 1990 In this issue we will try and answer some questions and the ones we can't we hope that our readers can. So enjoy. Dear TAP, I got TAP #97 last week and GREATLY enjoyed reading it. Highly informative. I wouldn't consider myself a hacker, but your article "A beginners guide to hacking" makes it very alluring (however, my hardware consists of a commodore 64 with a VIC-20 modem and cassette tape software). Is there any hope? Should i change modems? The other articles were also informative; I've already succeeded with the "Redneck Penny." Austin, TX Dear Austin, Issue 97 was our first attempt at the digest size issue and we liked it a lot better also. To answer your questions about a commodore. The modem that has the most hacking and phreaking software written for it is the c1670 modem. It is made by commodore. They range in price from 50-80 dollars. It depends on if you buy it locally or mail order. You would also want to get a 1541 disk drive, many programs won't work with a cassette tape. That should get you headed in the right direction. I also think you will find "Phoneman" a very good terminal program. It has many different tone emulators for colored boxes. Dear TAP, I was wondering if it's possible to make a universal garage door opener. Like the TV remotes that are universal and work on any TV. This would allow you to open someones garage without having a certain opener. Dayton, OH Dear Dayton, I don't know the exact frequencies that garage door openers run on, but i would assume that once found you could make an adjustable one with a knob of some kind to increase or decrease the range. If any reader can help please send the range the frequencies run in, or help on how this could be done. Dear TAP, I would like to know if it's possible to copy or pirate nintendo games? TAP Reply, I have heard that nintendo games use a means of copy protection. They have different eproms on about every 1,000 cartridges made. Thus making each lot different from all the others. If you had a way to copy the eproms and burn them into a blank one i guess it would work. But if they have copy protection built in you would have to find a way to bypass it. Dear TAP, Why don't you all put out an online type magazine like Phrack or ATI does? TAP Reply, We have been thinking about doing this for a few months now. As soon as all the staff has a computer and a modem we might attempt something. It would have to be different from all the rest though. Dear TAP, Was that really a picture of you guys on the cover of issue 99? TAP Reply, Nope, we found that picture on a telephone poll, but thought what the hell, it would make a fancy cover. Dear TAP, How come 2600 never mentions you as being another hacker publication in their mag? TAP Reply, I guess they have something against us. Maybe they don't know we exist. Ask Eric Corley i don't know... Dear TAP, How can you publish this stuff without the PHeds arresting you for doing it? TAP Reply, We gave them some donuts filled with brainwashing grape jelly and they don't know we exist. Dear TAP, How can you guys publish for free? I like the mag and enjoy reading it but wonder how you guys do it? Arizona Dear Arizona, Well as you might have seen, TAP is no longer free. It was jst to expensive to keep giving it away. Subscriptions are just $10.00 for 10 issues. USA price. Other rates have not been decided yet. Write for info. Dear TAP, I have written many articles how do i get them published in TAP magazine? Milwaukee, WI Dear Milwaukee, We would like to get many article from our readers. We can't print them all, some might not fit our format or be up to par with what we would use, but feel free to send us anything you think we might like reading. Newspaper clippings can also be useful to let us know whats going on in your area. Dear TAP, With all the stuff about Operation Sundevil why didn't you have any info on it? Dallas, TX Dear Dallas, We thought since it was in and on most everything else we would save you from the effort of reading it all over again. We cannot take a stand unless we know both sides of the story and with the federal cover ups and changing stories every week we just see it as another massive scare tactic. If for some reason you have been on an island or in a cave you can find info on Sundevil in CUD, 2600, Phrack, newspapers and just about every online service out there. Well that about wraps up the questions for now. Our next issue will be back to regular stories and columns. Until then may the feds be confused on the way to your door. */*/*/*/*/*/*/*/*/*/*/*/*/*/*/*/*/*/*/* Hacking Answering Machines 1990 */*/*/*/*/*/*/*/*/*/*/*/*/*/*/*/*/*/*/* by: Predat0r of Blitzkrieg Bbs 502/499-8933 AT&T reports that in the year 1990, 11 million people will buy an answering machine for their home use. In 1989, 10 million machines were sold. Everyone has called up a person at one time or another and got the old "leave your name at the beep" message. With this increase in homes using these machines there is also a new form of hacking developing. One of hacking an answering machine. Why would anyone even want to hack an answering machine and for what purpose? There are many reasons and things you can do once you have control of someone elses machine. If for some reason you need to spy on a business or person you can hack their machine and take control using the information for your own personal use. There is also the old "change the message" secret to make it say something to the effect of this line accepts all toll charges so you can bill third party calls to that number. You can also use an answering machine for your own personal use, as in making it your own voice mail type system for people to call. Only do this if you know someone is out of town. If they come home from shopping and find their machine changed it might cause problems. With these basic ideas in mind you can see hacking an answering machine could be very useful to certain individuals. How can a person hack an answering machine? Well most answering machines built now have remote access features which allow the owner, or anyone to call in and press a security code to play their messages. This is where the fun begins. Some older models don't have remote access so you cannot do anything to them. Also if you know someone has a machine but you call and it doesn't answer, let the phone ring about 15 times. This will tell the machine to turn itself on, so you can hack it. The actual number varies between machines. To practice hacking some machines i will show you how to get remote access on a few models. Just look and see what kind your friend has and hack it for starters. Record a Call- Model 2120 ------------------------- Call in and during the message or after the beep tone to leave a message enter the 3 digit security code. Which you must find yourself. This will rewind the tape and play all new messages. Press 2 to backspace and repeat the last message. Press 3 to fast foward the tape. Changing your message from remote. Call your phone and enter the secret code. After several rapid beeps enter your secret code again. After a short delay you will hear a long tone. After the tone ends begin speaking your message which may be 17 seconds in length. When finished press the second digit of your secret code to end. The machine will then save your message and play it back. To turn the unit on from remote let it ring 11 times then hangup. Or stay on and it will answer so you can access the machine. For express calls or frequent calls hit the second digit for two seconds to skip the out going message announcement. Goldstar- Models 6000/6100 -------------------------- Call and enter your 1 digit secret code after you hear the out going message announcement. The machine will then play back new messages. Hangup to save messages or after all messages have been played the machine will give a double beeptone, you may enter your code to erase all messages. You cannot change the out going message on this unit. Cobra- Model AN-8521 -------------------- For this machine there are 2 codes. Both are one digit in length. The first one is the play code. The second is to erase messages from remote. After the outgoing message and beeptone press the play code for 2 seconds to play messages. After each message ends there will be a single beep. At the end of all message it will beep twice. You may then do the following. Replay by pressing the play code again. Erase messages by pressing the erase code. Hang-up and save messages and continue to take additional calls. To turn this unit on from remote you must let it ring 16 times before it will activate. If it rings 10 times then you hear 3 beeps it is full and messages need to be erased. Uniden- Model AM 464 -------------------- This model is one of the more advanced when it comes to remote capabilities. The factory preset security code is 747. This can be changed to as many as five digits of your choice. To gain access from remote type your security code while the outgoing message is playing. Press 1 after hearing the tone and the machine will rewind and play your messages. To fast foward press 7, to resume normal playback press 8. To stop the messages from playing press 8 again. Press 8 to restart the messages or 1 to start from the beginning again. Press 9 to rewind and 8 to resume playing. If you rewind all the way it will beep twice. You need to press 1 to play messages.To save messages press 4. To erase press 6. To turn the machine off from remote press 5 after all messages have been played and the machine beeps twice. To turn the machine on from remote let the phone ring 12 to 14 times. The machine will beep and then you enter your remote code. This will then turn your machine to answer mode. This machine also has room monitor options. This allows you to listen to what is going on in the room of the machine. To do this call the machine enter your security code after the beep press 0. The monitor stays on for 60 seconds. You will be warned with 2 beeps at 45 seconds. To continue press 0 again.To change the outgoing message from remote erase all the messages. Then call back and enter your code after the tone press 3. It will beep again and you may then leave your new message. Press 3 when finished. To change the security code from remote after the beep press # then 1 after the next beep enter your new code followed by the # again. There is also a call break through where you enter 256 while the outgoing message is playing. This will alarm the persons in the house someone is calling with a series of loud beeps. Press the * key to stop. Code-a-phone Model 930 ---------------------- To access from remote call and enter your security code after the announcement and tone. Press your code for 3 full seconds. After the new messages have been played you will hear 2 tones. You may then save messages by pressing your code then hanging up. repeat by entering code wait for 4 tones then enter code again. To erase message hangup when the tape is done playing. To turn the machine on from remote call and let ring ten times. When the system answers it will have a two second tone. Press your security code. You will hear three double tones to let you know the system is on. Unisonic- Model 8720 -------------------- One digit code entered after the outgoing message and tone will allow you to hear messages. To change message wait till all new messages have been played 2 beep tones will be heard. Press code for four seconds. Two beeps will be heard then the tape will rewind and beep again. Now leave the new message. Press your code when finished to save new outgoing message. New message will play for you to hear. Panasonic- Model KX-T2427 ------------------------- Call and enter the three digit code during the outgoing message. Machine will beep once, then beep amount of times equal to messages. Then rewind and play messages. There will be three beeps after the last message. Six beeps means the tape is full. Press 2 to foward. Press 1 to rewind. Press 3 to reset machine and erase messages. To monitor the room press 5 after the beeps indicating the number of messages the machine has. Press 7 to change the outgoing message, it will beep a few quick times rewind then a long beep will be heard. Leave new message press 9 when finished. Press 0 right after the beep tones to shut the machine off. To turn the machine on let it ring 15 times then hangup after machine turns on. Panasonic- Model KX-T2385d -------------------------- During the outgoing message enter the 1 digit code. This will playback messages. Press the code again to rewind. After the messages have played the machine will beep three times. Press your code again and it will reset the machine. For remote turn on let phone ring 15 times. Then after the outgoing message hangup. AT&T- Model 1504 ---------------- Enter 2 digit code before or after announcement. System will beep after each message and five times when messages are done. Press the # key anytime to pause. Hanging up will save messages. Press 7 and it will rewind and play messages again. Press 5 to fast foward. Press 2 to rewind. Press 33 after all messages have been played to reset without saving messages. To record onto the tape press * after the system answers. This will then beep and you may leave a four minute message on the tape. Press # when done. This is not an outgoing message announcement, only a memo. To turn on from remote let ring ten times press 0 when system answers. To turn the system off dial and enter your code. Press 88 and it will shut the machine down. Phonemate- Model 4050 --------------------- Enter your 3 digit code during the outgoing message. Pressing * or # will allow you to scan through the messages. When finished pressing 1 will replay the messages. Pressing 2 will erase them. To turn on from remote let ring for 15 times. Then proceed with remote operations. Phonemate- Model 7200 --------------------- Enter 1 digit code during of after the outgoing message. A voice will tell you how many messages you have, then play them back for you. To rewind press your code and hold it for however long you want to rewind. Let go and it will resume playing. After the last message a voice will prompt you with a list of options. You have five seconds to respond or it will proceed to the next option. These are as follows. The first is hanging up to save messages. Next is enter code to replay messages. Next enter code to erase messages. Last is enter code to change greeting. Follow the voice and it will give you complete directions on exact steps to follow. To turn on from remote let ring ten times then hang up. If tape is full it will say sorry tape is full, enter code and erase messages. Spectra Phone- Model ITD300 --------------------------- Enter your 1 digit code after the greeting. Messages will play back. Hanging up will save them. Or wait for four beeps and press your code to replay them. To erase press your code after 2 beeps. To turn the machine on from remote let it ring 10 times. Notes: Outgoing message and greeting is what you hear when you first call. Code is your personal security code. Hacking answering machines can be very easy. It can also help you obtain valuable information. If you have a targeted machine you can try going to a store and saying you just bought one and it didn't have instructions in the box. They will usually give you a set or make copies for you. This basic guide is just to introduce you to answering machine hacking and changing the outgoing message and listening to messages left by callers. To keep your own machine safe purchase one with a changeable security code of 3 or more digits. Most home machines are of the 1 digit type and are easy to hack. I have no knwoledge of the laws concerning hacking into someones answering machine. I am sure once it becomes more common we will find out. Of course this article is for informational purposes only so you would never have to find out the actual laws. Taken from TAP Magazine Issue #100 NASA REVISED SPACE SHUTTLE MISSION STS-35 PRESS KIT DECEMBER 1990 PUBLIC AFFAIRS CONTACTS Mark Hess/Ed Campion Office of Space Flight NASA Headquarters, Washington, D.C. (Phone: 202/453-8536) Paula Cleggett-Haleim/Michael Braukus Office of Space Science and Applications NASA Headquarters, Washington, D.C. (Phone: 202/453-1548) Terri Sindelar Educational Affairs NASA Headquarters, Washington, D.C. (Phone: 202/453-8400) Nancy Lovato Ames-Dryden Flight Research Facility, Edwards, Calif. (Phone: 805/258-3448) Randee Exler Goddard Space Flight Center, Greenbelt, Md. (Phone: 301/286-7277) James Hartsfield Johnson Space Center, Houston (Phone: 713/483-5111) Lisa Malone/Pat Phillips Kennedy Space Center, Fla. (Phone: 407/867-2468) Jean Drummond Clough Langley Research Center, Hampton, Va. (Phone: 804/864-6122) David Drachlis/Jerry Berg Marshall Space Flight Center, Huntsville, Ala. (Phone: 205/544-0034) # # # # CONTENTS GENERAL RELEASE 1 SUMMARY OF MAJOR ACTIVITIES 2 STS-35 CARGO CONFIGURATION 3 STS-35 QUICK LOOK FACTS 4 GENERAL INFORMATION 5 TRAJECTORY SEQUENCE OF EVENTS 6 SPACE SHUTTLE ABORT MODES 6 PAYLOAD AND VEHICLE WEIGHTS 7 STS-35 PRELAUNCH PROCESSING 7 ASTRO-1 MISSION 8 ASTRO-1 OBSERVATORY 12 Hopkins Ultraviolet Telescope 12 Wisconsin Ultraviolet Photo-Polarimeter Experiment 15 Ultraviolet Imaging Telescope 17 BROAD BAND X-RAY TELESCOPE 19 ASTRO CARRIER SYSTEMS 22 ASTRO OPERATIONS 25 ASTRO GROUND CONTROL 27 ASTRO-1 HISTORY 29 SHUTTLE AMATEUR RADIO EXPERIMENT (SAREX) 30 STS-35 COLUMBIA SAREX FREQUENCIES 32 "SPACE CLASSROOM, ASSIGNMENT: THE STARS" 32 ORBITER EXPERIMENTS PROGRAM 33 STS-35 CREW BIOGRAPHIES 36 STS-35 MISSION MANAGEMENT 38 UPCOMING SPACE SHUTTLE FLIGHTS 40 PREVIOUS SPACE SHUTTLE FLIGHTS 41 # # # # GENERAL RELEASE RELEASE: 90-63 COLUMBIA TO FLY ASTRONOMY MISSION Highlighting mission STS-35, the 38th flight of the Space Shuttle and 10th mission of orbiter Columbia, will be around-the-clock observations by the seven-member crew using the ultraviolet astronomy observatory (Astro) and the Broad Band X-Ray Telescope (BBXRT). Both instruments are located in Columbia's payload bay and will be operated during 12-hour shifts by the crew. Above Earth's atmospheric interference, Astro-1 will observe and measure ultraviolet radiation from celestial objects. Astro-1 is the first in a series of missions that will make precise measurements of objects such as planets, stars and galaxies in relatively small fields of view. Liftoff of the 10th flight of Columbia is scheduled for the week of Dec. 2, 1990 from launch pad 39B at the Kennedy Space Center, Fla. Columbia will be placed into a 218 statute (190 nautical) mile circular orbit, inclined 28.5 degrees to the equator. Nominal mission duration is expected to be 9 days 21 hours 57 minutes. Landing will take place at Edwards Air Force Base, Calif. Astro-1 uses a Spacelab pallet system with an instrument pointing system and a cruciform structure for bearing the three ultraviolet instruments mounted in parallel configuration. The three instruments are the Hopkins Ultraviolet Telescope (HUT), the Wisconsin Ultraviolet Photo-polarimeter Experiment (WUPPE) and the Ultraviolet Imaging Telescope (UIT). The star tracker, which supports the instrument pointing system, also is mounted on the cruciform. HUT will study faint astronomical objects such as quasars, active galactic nuclei and supernova remnants in the little-explored ultraviolet range below 1200 Angstroms. It consists of a mirror that focuses on an aperture of a prime focus spectrograph. Observations of the outer planets of the solar system will be made to investigate aurorae and gain insight into the interaction of each planet's magnetosphere with the solar wind. WUPPE will measure the polarization of ultraviolet light from celestial objects such as hot stars, galactic nuclei and quasars. It uses two-mirror telescope optics in conjunction with a spectropolarimeter. This instrument will measure the polarization by splitting a beam of light into two mutually-perpendicular planes of polarization, passing the beams through a spectrometer and focusing the beams on two separate array detectors. UIT consists of a telescope and two image intensifiers with 70 mm film transports (1000 frames each). It will acquire images of faint objects in broad ultraviolet bands in the wavelength range of 1200 to 3200 Angstroms. This experiment also will investigate the present stellar content and history of star formation in galaxies, the nature of spiral structure and non-thermal sources in galaxies. Also in the payload bay is the Broad Band X-Ray Telescope which has two co-aligned imaging telescopes with cryogenically cooled lithium- drifted silicon detectors at each focus. Accurate pointing of the instrument is achieved by a two-axis pointing system (TAPS). BBXRT will study various targets, including active galaxies, clusters of galaxies, supernova remnants and stars. BBXRT will directly measure the amount of energy in electron volts of each X-ray detected. Astro observations will begin about 23 hours after Columbia has completed its maneuvering burn to circularize its orbit at 190 nautical miles. BBXRT will be activated approximately 13 hours after orbital insertion. Astro will be deactivated 12 hours before deorbit and BBXRT deactivation will be 4 hours before the deorbit burn. Columbia's middeck will carry the Shuttle Amateur Radio Experiment (SAREX) to communicate with amateur radio stations within line-of-sight of the orbiter in voice mode or data mode. This experiment has previously flown on STS-9 and STS-51F. Also on this mission, Columbia will function as the subject for ground sensor operations as part of the Air Force Maui Optical Site (AMOS) calibration test. Commander of the seven-member crew is Vance Brand. Pilot is Guy Gardner. STS-35 is Brand's fourth trip to space. He previously flew on the Apollo-Soyuz Test Project mission in 1975. He also commanded Shuttle missions STS-5 in November 1982 and STS-41B in February 1984. Gardner previously piloted STS-27 in December 1988. Mission Specialists are Mike Lounge, Jeffrey Hoffman and Robert Parker. Lounge previously flew on STS-51I in August 1985 and STS-26 in September 1988. Hoffman flew as a Mission Specialist on STS-51D in April 1985. Parker's previous spaceflight experience was STS-9 in November 1983. Payload Specialists Ronald Parise and Samuel Durrance round out the STS-35 crew. Both are making their first space flights. # # # # SUMMARY OF MAJOR ACTIVITIES Day One Ascent Post-insertion Unstow Cabin Astro/BBXRT Activation SAREX Setup DSO Day Two Astro/BBXRT Observations SAREX Day Three Astro/BBXRT Observations SAREX Day Four AMOS Astro/BBXRT Observations SAREX Day FIVE AMOS Astro/BBXRT Observations SAREX Space Classroom Day Six Astro/BBXRT Observations SAREX Day Seven Astro/BBXRT Observations RCS Hotfire Day Eight Astro/BBXRT Observations SAREX DTO FCS Checkout Day Nine Astro/BBXRT Observations SAREX SAREX Stow Astro/BBXRT Deactivation Cabin Stow Deorbit Burn Landing at Edwards AFB # # # # STS-35 QUICK LOOK Launch Date: December 2, 1990 Launch Window: 1:24 a.m. - 3:54 a.m. EST Launch Site: Kennedy Space Center, Fla. Launch Complex 39-B Orbiter: Columbia (OV-102) Altitude: 218 statute miles (190 nm) Inclination: 28.45 Duration: 9 days, 21 hours, 57 minutes Landing Date/Time: Dec. 11, 1990, 8:21 p.m. PST Primary Landing Site: Edwards Air Force Base, Calif. Abort Landing Sites: Return to Launch Site -- Kennedy Space Center, Fla. Trans-Atlantic Abort -- Banjul, The Gambia Abort Once Around -- Edwards AFB, Calif. Crew Vance D. Brand - Commander - Red/Blue Team Guy S. Gardner - Pilot - Red Team Jeffrey A. Hoffman - Mission Specialist 1/EV1 - Blue Team John M. "Mike" Lounge - Mission Specialist 2/EV2 - Blue Team Robert A.R. Parker - Mission Specialist 3 - Red Team Samuel T. Durrance - Payload Specialist 1 - Blue Team Ronald A. Parise - Payload Specialist 2 - Red Team Red Team shift is approximately 10:30 p.m. -- 10:30 a.m. EST Blue Team shift is approximately 10:30 a.m. -- 10:30 p.m. EST Cargo Bay Payloads: Ultraviolet Astronomy Telescope (Astro) Broad Band X-Ray Telescope (BBXRT) Middeck Payloads: Air Force Maui Optical Site (AMOS) Shuttle Amateur Radio Experiment (SAREX) # # # # GENERAL INFORMATION NASA Select Television Transmission NASA Select television is available on Satcom F-2R, Transponder 13, C-band located at 72 degrees west longitude, frequency 3960.0 MHz, vertical polarization, audio monaural 6.8 MHz. The schedule for tv transmissions from the orbiter and for the change-of-shift briefings from Johnson Space Center, Houston, will be available during the mission at Kennedy Space Center, Fla.; Marshall Space Flight Center, Huntsville, Ala.; Johnson Space Center; Goddard Space Flight Center, Greenbelt, Md. and NASA Headquarters, Washington, D.C. The schedule will be updated daily to reflect changes dictated by mission operations. TV schedules also may be obtained by calling COMSTOR, 713/483- 5817. COMSTOR is a computer data base service requiring the use of a telephone modem. Voice updates of the TV schedule may be obtained by dialing 202/755-1788. This service is updated daily at noon EDT. Status Reports Status reports on countdown and mission progress, on-orbit activities and landing operations will be produced by the appropriate NASA news center. Briefings An STS-35 mission press briefing schedule will be issued prior to launch. During the mission, flight control personnel will be on 8-hour shifts. Change-of-shift briefings by the off-going flight director will occur at approximately 8-hour intervals. TRAJECTORY SEQUENCE OF EVENTS --------------------------------------------------------------------------- RELATIVE EVENT MET VELOCITY MACH ALTITUDE (d:h:m:s) (fps) (ft) --------------------------------------------------------------------------- Launch 00/00:00:00 Begin Roll Maneuver 00/00:00:09 162 .14 613 End Roll Maneuver 00/00:00:16 340 .30 2,505 SSME Throttle Down to 70% 00/00:00:26 608 .54 6,759 Max. Dyn. Pressure (Max Q) 00/00:00:54 1,229 1.17 28,976 SSME Throttle Up to 104% 00/00:01:03 1,473 1.46 39,394 SRB Staging 00/00:02:05 4,203 3.87 150,267 Negative Return 00/00:03:58 6,940 7.58 309,526 Main Engine Cutoff (MECO) 00/00:08:31 24,439 22.99 360,922 Zero Thrust 00/00:08:37 24,556 22.73 363,937 ET Separation 00/00:08:49 OMS 2 Burn 00/00:40:22 Landing 09/21:57 Apogee, Perigee at MECO: 185 x 33 Apogee, Perigee post-OMS 2: 190 x 190 # # # # SPACE SHUTTLE ABORT MODES Space Shuttle launch abort philosophy aims toward safe and intact recovery of the flight crew, orbiter and its payload. Abort modes include: * Abort-To-Orbit (ATO) -- Partial loss of main engine thrust late enough to permit reaching a minimal 105-nautical mile orbit with orbital maneuvering system engines. * Abort-Once-Around (AOA) -- Earlier main engine shutdown with the capability to allow one orbit around before landing at Edwards Air Force Base, Calif.; White Sands Space Harbor (Northrup Strip), N.M.; or the Shuttle Landing Facility (SLF) at Kennedy Space Center, Fla.. * Trans-Atlantic Abort Landing (TAL) -- Loss of two main engines midway through powered flight would force a landing at Banjul, The Gambia; Ben Guerir, Morocco; or Moron, Spain. * Return-To-Launch-Site (RTLS) -- Early shutdown of one or more engines and without enough energy to reach Banjul would result in a pitch around and thrust back toward KSC until within gliding distance of the SLF. STS-35 contingency landing sites are Edwards AFB, White Sands, Kennedy Space Center, Banjul and Ben Guerir, Moron. # # # # PAYLOAD AND VEHICLE WEIGHTS Vehicle/Payload Weight (lbs) Orbiter Columbia empty 158,905 Ultraviolet Astronomy Telescope (Astro) 17,276 (IPS, igloo and 2 pallets) Astro Support Equipment 404 (middeck equipment) Broad Band X-Ray Telescope ((BBXRT) 8,650 (including TAPS and support equipment) Detailed Test Objectives (DTO) 274 Shuttle Amateur Radio Experiment (SAREX) 61 Total vehicle at SRB ignition 4,523,199 Orbiter and cargo at main engine cutoff 267,513 Orbiter landing weight 225,886 # # # # STS-35 PRELAUNCH PROCESSING Columbia's first launch attempt on May 29 was scrubbed because of higher than allowable concentrations of hydrogen near the 17-inch disconnect and in the aft compartment. Since that time, there have been several launch attempts and two tanking tests. After the first tanking test on June 6, officials decided to replace the 17-inch disconnect assemblies on both the orbiter and its external tank. Columbia was rolled back to the Vehicle Assembly Building June 11, demated from the external tank and transferred to the Orbiter Processing Facility. A new disconnect from the shuttle Endeavour was installed on Columbia and the orbiter and tank were remated. Columbia was rolled out to Pad 39-A on Aug. 9 for launch. The countdown began and launch was postponed on Aug. 30 to allow the replacement of an electronic box for the Broad Band X-Ray Telescope. Launch was scrubbed on Sept. 5 because of higher than allowable concentrations of hydrogen in the aft compartment. Another attempted launch occurred on Sept. 17, but again hydrogen was detected in the aft compartment. A board was appointed to find the cause of the leak. At the board's direction, several main propulsion system seals were replaced, many leak tests using gaseous helium were performed and various joints were retorqued. In addition, the team completed a thorough analysis of data collected from the tanking tests and reviewed all work performed on the orbiter's propulsion system since Columbia's last flight. The STS-35 vehicle was moved from Pad 39-A to 39-B on Oct. 8, following the successful launch of Discovery on Mission STS-41. The next day, Columbia was transferred back to the Vehicle Assembly Building because adverse weather prevented productive work in the aft compartment. On Oct. 14, the vehicle was rolled out to Pad 39-B, and specially outfitted for the successful tank ing test conducted Oct. 30. The successful tanking test paved the way for routine launch preparations leading up to Columbia's planned liftoff. # # # # THE ASTRO-1 MISSION Since the earliest days of astronomy, humankind has used the light from the stars to test their understanding of the universe. Now, an array of telescopes to be flown on the first Spacelab mission since 1985, will extend scientists' vision beyond the visible light to view some of the most energetic events in the universe. Astro-1 is the first Spacelab mission devoted to a single scientific discipline -- astrophysics. The observatory will operate from within the cargo bay of Space Shuttle Columbia on the STS-35 mission. Together, four telescopes will dissect ultraviolet light and X-rays from stars and galaxies, revealing the secrets of processes that emitted the radiation from thousands to even billions of years ago. Wherever it points, Astro promises to reveal an array of information. The Astro-1 Spacelab project is managed by NASA's Marshall Space Flight Center, Huntsville, Ala. Seeing the Universe Astronomy from the ground always has been hampered by the Earth's atmosphere. Even visible light is distorted and blurred by the motion of air masse, and visible light is just a small part of the radiation that virtually all objects in the sky emit. Other forms of radiation -- like cooler, low-energy infrared light and hotter, high-energy ultraviolet light and X-rays -- are largely absorbed by the atmosphere and never reach the ground. Seeing celestial objects in visible light alone is like looking at a painting in only one color. To appreciate fully the meaning of the painting, viewers must see it in all of its colors. The Astro-1 telescopes were constructed to add some of these "colors" to scientists' view of stars and galaxies. The telescopes' perch above the veil of Earth's atmosphere in Columbia's cargo bay will allow scientists to view radiation that is invisible on the ground. Three of Astro-1's telescopes will operate in the ultraviolet portion of the spectrum and one in the X-ray portion. One will take photographs; two will analyze the chemical composition, density and temperature of objects with a spectrograph; and the other will study the relative brightness and polarization (the study of light wavelength orientation) of celestial objects. Some sources will be among the faintest known, as faint as the glow of sunlight reflected back from interplanetary dust. By studying ultraviolet and X-rays, astronomers can see emissions from extremely hot gases, intense magnetic fields and other high-energy phenomena that are much fainter in visible and infrared light or in radio waves -- and which are crucial to a deeper understanding of the universe. Several space telescopes -- notably the Orbiting Astronomical Observatory-3 (Copernicus) launched in 1972, the International Ultraviolet Explorer launched in 1978 and the second High Energy Astronomy Observatory launched in 1979 -- opened the window in these exciting parts of the spectrum. The combined observations by Astro, the Hubble Space Telescope and ground-based observatories will provide astronomers with a more comprehensive view of the cosmos than ever before. What Astro-1 Will "See" The universe viewed by Astro will look strikingly different from the familiar night sky. Most stars will fade from view, too cool to emit significant ultraviolet radiation or X-rays. Yet, very young massive stars, very old stars, glowing nebulae, active galaxies and quasars will gleam brightly. Astro will make observations in this solar system. Astro will examine the chemistry of planetary atmospheres and the interactions of their magnetic fields. The Astro observatory will study comets as they interact with light and particles from the sun to produce bright, streaming tails. Stars Astro will peer far beyond this solar system to study many types of stars. The sun is only one of an estimated several hundred billion stars in the galaxy. Stars like the sun are the most common type: fiery spheres of gas, about 1 million times larger in volume than Earth, with nuclear furnaces that reach temperatures of millions of degrees. Today, current evidence indicates that the sun is a stable, middle- aged star, but some 5 billion years hence it will swell and swallow the inner planets including Earth. As a red giant, it may eject a shell of dust and gas, a planetary nebula. As the sun fades, it will collapse to an object no bigger than Earth, a dense, hot ember, a white dwarf. Astronomers predict that most stars may end their lives as white dwarfs, so it is important to study these stellar remains. White dwarfs emit most of their radiation in the ultraviolet, and one of Astro-1's main goals is to locate and examine white dwarfs in detail. Supernova Astro-1 instruments will locate hot, massive stars of all ages so that astronomers can study all phases of stellar evolution. Stars with 10 to 100 times more mass than the sun burn hydrogen rapidly until their cores collapse and they explode as supernovas, among the most powerful events in the universe. These stars are initially are very hot and emit mostly ultraviolet radiation. Astro will view the recent explosion, Supernova 1987A, which spewed stellar debris into space. Supernovas forge new elements, most of which are swept away in expanding shells of gas and debris heated by the shock waves from the blast. Astro-1 will look for supernova remnants which remain visible for thousands of years after a stellar death. Astro-1's ultraviolet and X-ray telescopes will provide information on element abundances, the physical conditions in the expanding gas and the structure of the interstellar medium. Neutron Stars, Pulsars, Black Holes After a supernova explosion, the stellar core sometimes collapses into a neutron star, the densest and tiniest of known stars, with mass comparable to the sun compacted into an area the size of a large city. Matter can become so dense that a sugar cube of neutron star material would weigh 100 million tons. Sometimes neutron stars are pulsars that emit beacons of radiation and appear to blink on and off as many as hundreds of times per second because they spin so rapidly. Scientists have theorized that some stars may collapse so far that they become black holes, objects so dense and gravitationally strong that neither matter nor light escape. Astro will look for the ultraviolet radiation and X-rays thought to be produced when hot, whirling matter is drawn into a black hole. Star Systems Few stars live in isolation; most are found in pairs or groups. Some stellar companions orbit each other and often pass so close that mass is transferred from one star to the other, producing large amounts of ultraviolet and X-ray radiation which Astro-1's four telescopes are designed to study. These binary star systems may consist of various combinations of objects including white dwarfs, neutron stars, and black holes. Star Clusters Stars may congregate in star clusters with anywhere from a few to millions of members. Often, there are so many stars in the core of a cluster, it is impossible to distinguish the visible light from individual stars. Because they shine brightly in the ultraviolet, Astro-1 can isolate the hot stars within clusters. The clusters are excellent laboratories for studying stellar evolution because the stars residing there formed from the same material at nearly the same time. However, within a single cluster, stars of different masses evolve at different rates. Stellar evolution can be studied by looking at clusters of different ages. Each cluster of a given age provides a snapshot of what is happening as a function of stellar mass. By examining young clusters (less than 1 million years old) and comparing them to old clusters (1 billion years old), scientists can piece together what happens over a long time. Interstellar Medium The space between stars is filled with dust and gas, some of which will condense to become future stars and planets. This interstellar medium is composed chiefly of hydrogen with traces of heavier elements and has a typical density of one atom per thimbleful of space. Astro-1 will be able to measure the properties of this material more accurately by studying how it affects the light from distant stars. For the most part, the interstellar medium is relatively cool, but it includes pockets of hot matter as well. Dense clouds of dust that surround stars and scatter and reflect light are called reflection nebulae. These are often illuminated by hot, young stars in stellar nurseries hidden within the clouds. Ultraviolet observations will reveal the features of stars hidden by the dust as well as the size and composition of the dust grains. Other Galaxies Beyond the Milky Way are at least a hundred billion more galaxies, many with hundreds of billions of stars. They contain most of the visible matter in the universe and are often found in clusters of galaxies that have tens to thousands of members. X-ray and ultraviolet emission will allow scientists to study the hottest, most active regions of these galaxies as well as the intergalactic medium, the hot gas between the galaxies in a cluster. Galaxies have a variety of shapes and sizes: gigantic spirals like the Milky Way, egg-shaped elliptical and irregular shapes with no preferred form. Astro will survey the different types of galaxies and study their evolution. The nearby galaxies will appear as they were millions of years ago, and Astro will see the most distant ones as they were billions of years ago. By comparing these galaxies, scientists can trace the history of the universe. Quasars Some galaxies are in the process of violent change. Such active galaxies have central regions (nuclei) that emit huge amounts of energy; their ultraviolet and X-ray emission may help us identify their source of power. Astro-1's ultraviolet and X-ray telescopes will detect quasars, very distant compact objects that radiate more energy than 100 normal galaxies. Quasars may be the nuclei of ancient active galaxies. Strong X-ray and ultraviolet radiation arising in the central cores of these powerful objects may help scientists discover what these objects really are. This overview is the known universe today, but many of these ideas are only predictions based on theory and a few observations. Scientists still lack the definitive observations needed to confirm or refute many of these theories. Scientists do not know the exact size of the universe or its age. Scientists have never definitely seen a black hole, and they continue to question the nature of quasars. To understand these mysteries, scientists need to see the universe in all its splendor. Astro is part of NASA's strategy to study the universe across the electromagnetic spectrum, in all wavelengths. THE ASTRO-1 OBSERVATORY The Astro-1 observatory is a compliment of four telescopes. Though each instrument is uniquely designed to address specific questions in ultraviolet and X-ray astronomy, when used in concert, the capability of each is enhanced. The synergistic use of Astro-1's instruments for joint observations serves to make Astro-1 an exceptionally powerful facility. The Astro-1 observatory has three ultraviolet-sensitive instruments: o Hopkins Ultraviolet Telescope (HUT) uses a spectrograph to examine faint astronomical objects such as quasars, active galactic nuclei and normal galaxies in the far ultraviolet. o Ultraviolet Imaging Telescope (UIT) will take wide-field-of-view photographs of objects such as hot stars and galaxies in broad ultraviolet wavelength bands. o Wisconsin Ultraviolet Photo-Polarimeter Experiment (WUPPE) will study the ultraviolet polarization of hot stars, galactic nuclei and quasars. These instruments working together will make 200 to 300 observations during the STS-35 mission. The Astro ultraviolet telescopes are mounted on a common pointing system in the cargo bay of the Space Shuttle. The grouped telescopes will be pointed in the same direction at the same time, so simultaneous photographs, spectra and polarization studies will be available for each object observed. The telescopes will be operated by Columbia's crew. A fourth Astro instrument, the Broad Band X-Ray Telescope (BBXRT), will view high-energy objects such as active galaxies, quasars and supernovas. This telescope is mounted on a separate pointing system secured by a support structure in the cargo bay. For joint observations, BBXRT can be aligned with the ultraviolet telescopes to see the same objects, but it also can be pointed independently to view other X-ray sources. BBXRT will be operated remotely by ground controllers. Since the ultraviolet telescopes and the X-ray telescope are mounted on different support structures, they can be reflown together or separately. The Hopkins Ultraviolet Telescope The Hopkins Ultraviolet Telescope is the first major telescope capable of studying far ultraviolet (FUV) and extreme ultraviolet (EUV) radiation from a wide variety of objects in space. HUT's observations will provide new information on the evolution of galaxies and quasars, the physical properties of extremely hot stars and the characteristics of accretion disks (hot, swirling matter transferred from one star to another) around white dwarfs, neutron stars and black holes. HUT will make the first observations of a wide variety of astronomical objects in the far ultraviolet region below 1,200 Angstroms (A) and will pioneer the detailed study of stars in the extreme ultraviolet band. Ultraviolet radiation at wavelengths shorter than 912 A is absorbed by hydrogen, the most abundant element in the universe. HUT will allow astronomers, in some instances along unobserved lines of sight, to see beyond this cutoff, called the Lyman limit, because the radiation from the most distant and rapidly receding objects, such as very bright quasars, is shifted toward longer wavelengths. HUT was designed and built by the Center for Astrophysical Sciences and the Applied Physics Laboratory of The Johns Hopkins University in Baltimore, Md. Its 36-inch mirror is coated with the rare element iridium, a member of the platinum family, capable of reflecting far and extreme ultraviolet light. The mirror, located at the aft end of the telescope, focuses incoming light from a celestial source back to a spectrograph mounted behind the telescope. A grating within the spectrograph separates the light, like a rainbow, into its component wavelengths. The strengths of those wavelengths tell scientists how much of certain elements are present. The ratio of the spectral lines reveal a source's temperature and density. The shape of the spectrum shows the physical processes occurring in a source. The spectrograph is equipped with a variety of light-admitting slits or apertures. The science team will use different apertures to accomplish different goals in their observation. The longest slit has a field of view of 2 arc minutes, about 1/15th the apparent diameter of the moon. HUT is fitted with an electronic detector system. Its data recordings are processed by an onboard computer system and relayed to the ground for later analysis. Johns Hopkins scientists conceived HUT to take ultraviolet astronomy beyond the brief studies previously conducted with rocket- borne telescopes. A typical rocket flight might gather 300 seconds of data on a single object. HUT will collect more than 300,000 seconds of data on nearly 200 objects during the Astro-1 mission, ranging from objects in the solar system to quasars billions of light-years distant. HUT Vital Statistics Sponsoring Institution: The Johns Hopkins University, Baltimore, Md. Principal Investigator: Dr. Arthur F. Davidsen Telescope Optics: 36 in. aperture, f/2 focal ratio, iridium-coated paraboloid mirror Instrument: Prime Focus Rowland Circle Spectrograph with microchannel plate intensifier and electronic diode array detector Field of View of Guide TV: 10 arc minutes Spectral Resolution: 3.0 A Wavelength Range: 850 A to 1,850 A (First Order) 425 A to 925 A (Second Order) Weight: 1,736 lb Size: 44 inches in diameter 12.4 ft. in length Wisconsin Ultraviolet Photo-Polarimeter Experiment Any star, except for our sun, is so distant that it appears as only a point of light and surface details cannot be seen. If the light from objects is polarized, it can tell scientists something about the source's geometry, the physical conditions at the source and the reflecting properties of tiny particles in the interstellar medium along the radiation's path. The Wisconsin Ultraviolet Photo-Polarimeter Experiment (WUPPE), developed by the Space Astronomy Lab at the University of Wisconsin- Madison, is designed to measure polarization and intensity of ultraviolet radiation from celestial objects. WUPPE is a 20-inch telescope with a 5.5-arc-minute field of view. WUPPE is fitted with a spectropolarimeter, an instrument that records both the spectrum and the polarization of the ultraviolet light gathered by the telescope. Light will pass through sophisticated filters, akin to Polaroid sunglasses, before reaching the detector. Measurements then will be transmitted electronically to the ground. Photometry is the measurement of the intensity (brightness) of the light, while polarization is the measurement of the orientation (direction) of the oscillating light wave. Usually waves of light move randomly -- up, down, back, forward and diagonally. When light is polarized, all the waves oscillate in a single plane. Light that is scattered, like sunlight reflecting off water, is often polarized. Astro-1 astronomers expect to learn about ultraviolet light that is scattered by dust strewn among stars and galaxies. They also can learn about the geometry of stars and other objects by studying their polarization. To date, virtually no observations of polarization of astronomical sources in the ultraviolet have been carried out. WUPPE measures the polarization by splitting a beam of radiation into two perpendicular planes of polarization, passing the beams through a spectrometer and focusing the beams on two separate array detectors. In the ultraviolet spectrum, both photometry and polarization are extremely difficult measurements to achieve with the high degree of precision required for astronomical studies. To develop an instrument that could make these delicate measurements required an unusually innovative and advanced technical effort. Thus, the WUPPE investigation is a pioneering foray with a new technique. The targets of WUPPE investigations are primarily in the Milky Way galaxy and beyond, for which comparative data exist in other wavelengths. Like the Hopkins Ultraviolet Telescope, WUPPE also makes spectroscopic observations of hot stars, galactic nuclei and quasars. Operating at ultraviolet wavelengths that are mostly longer than those observed by HUT (but with some useful overlap), WUPPE provides chemical composition and physical information on celestial targets that that give off a significant amount of radiation in the 1,400 to 3,200 A range. WUPPE Vital Statistics Sponsoring Institution: University of Wisconsin, Madison Principal Investigator: Dr. Arthur D. Code Telescope Optics: Cassegrain (two-mirror) system, f/10 focal ratio Instrument: Spectropolarimeter with dual electronic diode array detectors Primary Mirror Size: 20 in. diameter 279 sq.* in. area Field of View: 3.3 x 4.4 arc minutes Spectral Resolution: 6 Angstroms Wavelength Range: 1,400 to 3,200 Angstroms Magnitude Limit: 16 Weight: 981 lb Size: 28 inches in diameter 12.4 ft. in length * This and subsequent changes were made to avoid confusion since the computer will not create exponents for cm2 or the circle over the A for Angstrom. The Ultraviolet ImagingTelescope In the 20 years that astronomical observations have been made from space, no high-resolution ultraviolet photographs of objects other than the sun have been made. Nonetheless, the brief glimpses of the ultraviolet sky have led to important discoveries in spiral galaxies, globular clusters, white dwarf stars and other areas. Deep, wide-field imaging is a primary means by which fundamentally new phenomena or important examples of known classes of astrophysical objects will be recognized in the ultraviolet. The Ultraviolet Imaging Telescope (UIT), developed at NASA's Goddard Space Flight Center in Greenbelt, Md., is the key instrument for these investigations. UIT is a powerful combination of telescope, image intensifier and camera. It is a 15.2-inch Ritchey Chretien telescope with two selectable cameras mounted behind the primary mirror. Each camera has a six- position filter wheel, a two-stage magnetically focused image tube and a 70-mm film transport, fiber optically coupled to each image tube. One camera is designed to operate in the 1200 - 1700 Angstrom region and the other in the 1250-3200 Angstrom region. Unlike data from the other Astro instruments, which will be electronically transmitted to the ground, UIT images will be recorded directly onto a very sensitive astronomical film for later development after Columbia lands. UIT has enough film to make 2,000 exposures. A series of 11 different filters allows specific regions of the ultraviolet spectrum to be isolated for energy-distribution studies. After development, each image frame will be electronically digitized to form 2,048 x 2,048 picture elements, or pixels, then analyzed further with computers. UIT has a 15-inch diameter mirror with a 40-arc-minute field of view -- about 25 percent wider than the apparent diameter of the full moon. UIT has the largest field of view of any sensitive UV imaging instrument planned for flight in the 1990s. It will photograph nearby galaxies, large clusters of stars and distant clusters of galaxies. A 30-minute exposure (the length of one orbital night) will record a blue star of 25th magnitude, a star about 100 million times fainter than the faintest star visible to the naked eye on a dark, clear night. Since UIT makes longer exposures than previous instruments, fainter objects will be visible in the images. The instrument favors the detection of hot objects which emit most of their energy in the ultraviolet. Common examples span the evolutionary history of stars -- massive stars and stars in the final stages of stellar evolution (white dwarfs). Images of numerous relatively cool stars that do not radiate much in the ultraviolet are suppressed, and UV sources stand out clearly. The UIT's field of view is wide enough to encompass entire galaxies, star clusters and distant clusters of galaxies. This deep survey mode will reveal many new, exciting objects to be studied further by NASA's Hubble Space Telescope. Although the Hubble Space Telescope will have a much higher magnification and record much fainter stars, the UIT will photograph much larger regions all at once. In addition, the UIT will suffer much less interference from visible light, since it is provided with "solar blind" detectors. For certain classes of targets, such as diffuse, ultraviolet-emitting or ultraviolet-scattering nebulae, UIT may be a more sensitive imager. A wide selection of astronomical objects will be studied in this first deep survey of cosmic phenomena in the ultraviolet. The UIT is expected to target hot stars in globular clusters to help explain how stars evolve. Another experiment may help astronomers learn whether properties and distribution of interstellar dust are the same in all galaxies. High-priority objects are Supernova 1987A and vicinity, star clusters, planetary nebulae and supernova remnants, spiral and "normal" galaxies, the interstellar medium of other galaxies and clusters of galaxies. UIT Vital Statistics Sponsoring Institution: NASA Goddard Space Flight Center (GSFC), Greenbelt, Md. Principal Investigator: Theodore P. Stecher (NASA GSFC) Telescope Optics: Ritchey-Chretien (variation of Cassegrain two-mirror system with correction over wide field of view) Aperture: 15 in. Focal Ratio: f/9 Field of View: 40 arc minutes Angular Resolution: 2 arc seconds Wavelength Range: 1,200 A to 3,200 A Magnitude Limit: 25 Filters: 2 filter wheels, 6 filters each Detectors: Two image intensifiers with 70-mm film, 1,000 frames each; IIaO astronomical film Exposure Time: Up to 30 minutes Weight: 1,043 lb Size: 32 inches in diameter 12.4 ft. in length THE BROAD BAND X-RAY TELESCOPE The Broad Band X-Ray Telescope (BBXRT) will provide astronomers with the first high-quality spectra of many of the X-ray sources discovered with the High Energy Astronomy Observatory 2, better known as the Einstein Observatory, launched in the late 1970s. BBXRT, developed at NASA's Goddard Space Flight Center in Greenbelt, Md., uses mirrors and advanced solid-state detectors as spectrometers to measure the energy of individual X-ray photons. These energies produce a spectrum that reveals the chemistry, structure and dynamics of a source. BBXRT is actually two 8-inch telescopes each with a 17 arc-minute field of view (more than half the angular width of the moon). The two identical telescopes are used to focus X-rays onto solid-state spectrometers which measure photon energy in electron volts in the "soft" X-ray region, from 380 to 12,000 eV. The use of two telescopes doubles the number of photons that are detected and also provides redundancy in case of a failure. X-ray telescopes are difficult to construct because X-ray photons are so energetic that they penetrate mirrors and are absorbed. A mirror surface reflects X-rays only if it is very smooth and the photons strike it at a very shallow angle. Because such small grazing angles are needed, the reflectors must be very long to intercept many of the incident X-rays. Since even shallower angles are required to detect higher-energy X-rays, telescopes effective at high energies need very large reflecting surfaces. Traditionally, X-ray telescopes have used massive, finely polished reflectors that were expensive to construct and did not efficiently use the available aperture. The mirror technology developed for BBXRT consists of very thin pieces of gold-coated aluminum foil that require no polishing and can be nested very closely together to reflect a large fraction of the X-rays entering the telescope. Because its reflecting surfaces can be made so easily, BBXRT can afford to have mirrors using the very shallow grazing angles necessary to reflect high-energy photons. In fact, BBXRT is one of the first telescopes to observe astronomical targets that emit X-rays above approximately 4,000 electron volts. The telescope will provide information on the chemistry, temperature and structure of some of the most unusual and interesting objects in the universe. BBXRT can see fainter and more energetic objects than any yet studied. It will look for signs of heavy elements such as iron, oxygen, silicon and calcium. These elements usually are formed in exploding stars and during mysterious events occurring at the core of galaxies and other exotic objects. BBXRT will be used to study a variety of sources, but a major goal is to increase our understanding of active galactic nuclei and quasars. Many astronomers believe that the two are very similar objects that contain an extremely luminous source at the nucleus of an otherwise relatively normal galaxy. The central source in quasars is so luminous that the host galaxy is difficult to detect. X-rays are expected to be emitted near the central engine of these objects, and astronomers will examine X-ray spectra and their variations to understand the phenomena at the heart of quasars. Investigators are interested in clusters of galaxies, congregations of tens or thousands of galaxies grouped together within a few million light- years of each other. When viewed in visible light, emissions from individual galaxies are dominant, but X-rays are emitted primarily from hot gas between the galaxies. In fact, theories and observations indicate that there should be about as much matter in the hot gas as in the galaxies, but all this material has not been seen yet. BBXRT observations will enable scientists to calculate the total mass of a cluster and deduce the amount of "dark" matter. A star's death, a supernova, heats the region of the galaxy near the explosion so that it glows in X-rays. Scientists believe that heavy elements such as iron are manufactured and dispersed into the interstellar medium by supernovas. The blast or shock wave may produce energetic cosmic ray particles that travel on endless journeys throughout the universe and instigate the formation of new stars. BBXRT detects young supernova remnants (less than 10,000 years old) which are still relatively hot. Elements will be identified, and the shock wave's movement and structure will be examined. BBXRT was not part of the originally selected ASTRO payload. It was added to the mission after the appearance of Supernova 1987A in February 1987, to obtain vital scientific information about the supernova. In addition, data gathered by BBXRT on other objects will enhance studies that would otherwise be limited to data gathered with the three ultraviolet telescopes. BBXRT Vital Statistics Sponsoring Institution: NASA Goddard Space Flight Center, Greenbelt, Md. Principal Investigator: Dr. Peter J. Serlemitsos Telescope Optics: Two co-aligned X-ray telescopes with cooled segmented lithium-drifted silicon solid-state detectors in the focal planes Focal Length: 12.5 ft. each, detection area 0.16 in. diameter pixel Focal Plane Scale: 0.9 arc minutes per mm Field of View: 4.5 arc minutes (central element); 17 arc minutes (overall) Energy Band: 0.3 to 12 keV Effective Area: 765 cm2 at 1.5 keV, 300 cm2 at 7 keV Energy Resolution: 0.09 keV at 1 keV, 0.15 keV at 6 keV Weight: 1,500 lb (680.4 kg) Size: 40 inches in diameter 166 inches in length ASTRO CARRIER SYSTEMS The Astro observatory is made up of three co-aligned ultraviolet telescopes carried by Spacelab and one X-ray telescope mounted on the Two-Axis Pointing System (TAPS) and a special structure. Each telescope was independently designed, but all work together as elements of a single observatory. The carriers provide stable platforms and pointing systems that allow the ultraviolet and X-ray telescopes to observe the same target. However, having two separate pointing systems gives investigators the flexibility to point the ultraviolet telescopes at one target while the X-ray telescope is aimed at another. Spacelab The three ultraviolet telescopes are supported by Spacelab hardware. Spacelab is a set of modular components developed by the European Space Agency and managed by the NASA Marshall Space Flight Center, Hunstville, Ala. For each Spacelab payload, specific standardized parts are combined to create a unique design. Elements are anchored within the cargo bay, transforming it into a short-term laboratory in space. Spacelab elements used to support the Astro observatory include two pallets, a pressurized igloo to house subsystem equipment and the Instrument Pointing System. The pressurized Spacelab laboratory module will not be used for Astro. Rather, astronauts and payload specialists will operate the payload from the aft flight deck of the orbiter Columbia. Pallets The ultraviolet telescopes and the Instrument Pointing System are mounted on two Spacelab pallets -- large, uncovered, unpressurized platforms designed to support scientific instruments that require direct exposure to space. Each individual pallet is 10 feet long and 13 feet wide. The basic pallet structure is made up of five parallel U-shaped frames. Twenty-four inner and 24 outer panels, made of aluminum alloy honeycomb, cover the frame. The inner panels are equipped with threaded inserts so that payload and subsystem equipment can be attached. Twenty-four standard hard points, made of chromium-plated titanium casting, are provided for payloads which exceed acceptable loading of the inner pallets. Pallets are more than a platform for mounting instrumentation. With an igloo attached, they also can cool equipment, provide electrical power and furnish connections for commanding and acquiring data from experiments. Cable ducts and cable support trays can be bolted to the forward and aft frame of each pallet to support and route electrical cables to and from the experiments and the subsystem equipment mounted on the pallet. The ducts are made of aluminum alloy sheet metal. In addition to basic utilities, some special accommodations are available for pallet-mounted experiments. For Astro-1, two pallets are connected together to form a single rigid structure called a pallet train. Twelve joints are used to connect the two pallets. Igloo Normally Spacelab subsystem equipment is housed in the core segment of the pressurized laboratory module. However, in "pallet only" configurations such as Astro, the subsystems are located in a supply module called the igloo. It provides a pressurized compartment in which Spacelab subsystem equipment can be mounted in a dry-air environment at normal Earth atmospheric pressure, as required by their design. The subsystems provide such services as cooling, electrical power and connections for commanding and acquiring data from the instruments. The igloo is attached vertically to the forward end frame of the first pallet. Its outer dimensions are approximately 7.9 feet in height and 3.6 feet in diameter. The igloo is a closed cylindrical shell made of aluminum alloy and covered with multi-layer insulation. A removable cover allows full access to the interior. The igloo consists of two parts. The primary structure -- an exterior cannister -- is a cylindrical, locally stiffened shell made of forged aluminum alloy rings and closed at one end. The other end has a mounting flange for the cover. A seal is inserted when the two structures are joined together mechanically to form a pressure-tight assembly. There are external fittings on the cannister for fastening it to the pallet, handling and transportation on the ground, and thermal control insulation. Two feed-through plates accommodate utility lines and a pressure relief valve. Facilities on the inside of the cannister are provided for mounting subsystem equipment and the interior igloo structure. The cover is also a cylindrical shell, made of welded aluminum alloy and closed at one end. The igloo has about 77.7 cubic feet of interior space for subsystems. Subsystem equipment is mounted on an interior or secondary structure which also acts as a guide for the removal or replacement of the cover. The secondary structure is hinge-fastened to the primary structure, allowing access to the bottom of the secondary structure and to equipment mounted within the primary structure. Instrument Pointing System Telescopes such as those aboard Astro-1 must be pointed with very high accuracy and stability at the objects which they are to view. The Spacelab Instrument Pointing System provides precision pointing for a wide range of payloads, including large single instruments or clusters of instruments. The pointing mechanism can accommodate instruments weighing up to 15,432 pounds and can point them to within 2 arc seconds and hold them on target to within 1.2 arc seconds. The combined weight of the ultraviolet telescopes and the structure which holds them together is 9,131 pounds. The Instrument Pointing System consists of a three-axis gimbal system mounted on a gimbal support structure connected to the pallet at one end and the aft end of the payload at the other, a payload clamping system for support of the mounted experiment during launch and landing and a control system based on the inertial reference of a three-axis gyro package and operated by a gimbal-mounted microcomputer. Three bearing-drive units on the gimbal system allow the payload to be pointed on three axes: elevation (back and forth), cross-elevation (side to side) and azimuth (roll), allowing it to point in a 22-degree circle around a its straight-up position. The pointing system may be maneuvered at a rate of up to one degree per second, which is five times as fast as the Shuttle orbiter's maneuvering rate. The operating modes of the different scientific investigations vary considerably. Some require manual control capability, others slow scan mapping, still others high angular rates and accelerations. Performance in all these modes requires flexibility achieved with computer software. The Instrument Pointing System is controlled through the Spacelab subsystem computer and a data-display unit and keyboard. It can be operated either automatically or by the Spacelab crew from the module (when used) and also from the payload station in the orbiter aft flight deck. In addition to the drive units, Instrument Pointing System structural hardware includes a payload/gimbal separation mechanism, replaceable extension column, emergency jettisoning device, support structure and rails and a thermal control system. The gimbal structure itself is minimal, consisting only of a yoke and inner and outer gimbals to which the payload is attached by the payload-mounted integration ring. An optical sensor package is used for attitude correction