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Lyon-Meudon Extragalactic DAtabase (LEDA) Created in 1983, LEDA is the oldest Extragalactic Database. It gives more than 60 of the most important parameters for about 100.000 galaxies. It provides charts and images through an X11 interface. In addition, a batch mode is available and also a very powerful SQL-like query language.
INSTRUCTIONS FOR USE Last update: March,1994 # LYON MEUDON ### EXTRAGALACTIC ##### DATABASE ####### ######### ########### ############# ############### #### ############ ##### ############ ##### ############ ########## ############## ########### ## ##### ############ ##### #### #### ##### ##### # ##### ### ###### ##### ##### # ##### #### ####### ##### ######### ##### ### ######## ##### ######### ##### ### ### ##### ##### ##### # ##### ### ########### ###### ## ##### ## ##### #### ### ##### ############ ############ ##### #### ### ##### ############## ############## ########### ###### ####### #### ############# #### ############# ##### ############## ####### ################# ############# ####################### HOW TO CONNECT ============== >From an INTERNET site ===================== Enter : telnet lmc.univ-lyon1.fr (or : telnet 134.214.4.7) login : leda >From an SPAN site ================= Enter : set host ciripa login : lmc.univ-lyon1.fr! (or : login : 134.214.4.7!) login : leda INTRODUCTION ============ LEDA has been the first Extragalactic Database. It was created in 1983 at Lyon Observatory. Since this time, the database has been continuously updated. The main idea is to collect raw measurements (coming directly from observations) and to archive them. Mean homogenized data are calculated in the same spirit as those used by de Vaucouleurs et al. when publishing the series of Bright Galaxy Catalogues (RC1, RC2, RC3). In fact, RC3 was created using the LEDA database. Two kinds of terminal are supported: text terminal (VT100) or graphic terminal (X11). The second one gives access to the full on-line graphic capabilities. An eight-bit-color screen and a minimum of 4 Mbyte memory are needed. The result of any request will be sent to you via e-mail. So, please, provide your e-mail address carefully. You may give an alias after your e-mail address. This alias will be kept by the system for easier future connections. example: jdoe@lmc.univ.lyon1.fr dodo (dodo is the alias) You will receive an ASCII file containing all information you selected during the connection. Charts and images will also be sent in ASCII format as Postscript files. These files can be sent to a laser printer supporting Postscript language (Postscript is a Trade mark of Adobe Corporation). Note that before sending such Postscript files to your laser printer you must remove the heading of the e-mail message. This can be done easily using mail capabilities (option: w message# file_name). Note that, at certain sites blank lines have to be removed from the beginning of the file. When using an X11 terminal charts and images are displayed directly on the screen and sent as Postscript files only when the user has pushed the 'SAVE' button. DIAGRAM OF MENUS ================ The structure of menus is the following in both VT100 and X11: MAIN MENU: Single object : Explore raw data : Explore mean data Several objects : Select from a list of names : SQL-like selection 2D-information : Charts : Images Information : Instructions for use : News : LEDA's team Exit : Give comments Except for the SQL-like option, NO PRIOR KNOWLEDGE IS NECESSARY to use LEDA interactively. Generally, you just have to follow on-line instructions. However, it could be helpful to explain how to designate an object. You may designate an object with: 1) A Name written in a free format (e.g.: M31 or m31 or messier 31; NGC224 or n 224 etc...) 2) Coordinates in a free format, for the epoch you have chosen (e.g. for R.A.: 12h30.0 or 12.5 or 12 h 30mn 0 s etc...) WARNING: Do not use e.g. '.3' but '0.3'. 3) the internal record number. This internal record number is especially useful for multiple objects. (e.g., If you ask UGC 1, LEDA gives internal record number for both galaxies covered by the name UGC 1) Now let us give more details about two powerful options: SQL-like language and BATCH mode. SQL-like language ================= The Standard Query Language has been developed by IBM (SQL is a trade mark of IBM corporation). The LEDA query language (LQL) is somewhat similar. The principle consists in giving a sentence which describes the request. The structure of this sentence is always the same: select (parameters desired for output) where (conditions) end ------ ----- --- The parameters you desire in the output file are simply given as a list of parameter names (or a combination of them), each name being separated by a comma. ex: select ident1,al2000,de2000,logd25 where (conditions) end ------ ----- --- The authorized parameter names are given below. The elementary conditions are built using operators like >, <, =, (, ) and operands (+,-,*,/,^ (exponent), & (exist), not(), log(), ln(), exp(), sqrt(), sin(), cos(), tan(), abs()). Note that you must put character strings between apostrophes (') (e.g., typ='E') Here are some examples: select ident1,logd25 where (w20>200 and w20<300) end select ident1 where &w20 or &w50 end select pgc,al2000,de2000 where (bt+5*logd25)<20 end select pgc,al2000,de2000 where al2000<3.0 and al2000>2.0 end select all where w20 > 500 and w20 < 550 end select pgc,typ where typ='E' and bt<10 end select pgc,(bt+5*logd25) where (bt+5*logd25)<20 end select pgc where ring='R' and multiple='M' end select pgc,abs(w20-w50) where &w20 and &w50 and abs(w20-w50)>100 end select ident1 where &w20 and not(&w50) end The most important thing to know is the name and definition of each parameter. The complete list is given below and the detailed description of the way they were calculated is given in ANNEX B: al1950 R.A. (B1950) (decimal hours) de1950 DEC. (B1950) (decimal degrees) ipad '*' for coordinates better than 10" *** alphabetical *** al2000 R.A. (J2000) (decimal hours) de2000 DEC. (J2000) (decimal degrees) l2 galactic longitude (degrees) b2 galactic latitude (degrees) sgl supergalactic longitude (degrees) sgb supergalactic latitude (degrees) pgc PGC name *** alphabetical ** ident1 1st name (NGC,IC,UGC,ESO...) *** alphabetical ** pa position angle (N->E) in degrees typ morphological type (e.g. 'E','Sab','SBa','SO') *** alphabetical ** ring 'R' for Ring galaxies, otherwise ' ' (blank) *** alphabetical ** multiple 'M' for multiple galaxies, otherwise ' ' (blank) *** alphabetical ** compact 'C' for compact, 'D' for diffuse, otherwise ' ' *** alphabetical ** t morphological type code (-5 to 10) st mean error on t lc luminosity class (1 to 11) slc mean error on lc logd25 log10 of isophotal diameter (d25 in 0.1') slogd25 mean error on logd25 logr25 log10 of the axis ratio (major/minor axis) slogr25 mean error on logr25 brief effective surface brightness (mag.arcsec-2) sbrief mean error on brief bt total B-magnitude sbt mean error on bt ubt (U-B)T bvt (B-V)T ube (U-B)e bve (B-V)e w20 21-cm line width at 20% of the peak (in km/s) sw20 mean error on w20 w50 21-cm line width at 50% of the peak (in km/s) sw50 mean error on w50 logs log10 of the central velocity dispersion (s in km/s) slogs mean error on logs m21 HI-magnitude sm21 mean error on m21 mfir far-infrared magnitude vrad radio heliocentric radial velocity in km/s svrad mean error on vrad vopt optical heliocentric radial velocity in km/s svopt mean error on vopt v mean heliocentric radial velocity in km/s sv mean error on v lgg Lyon's galaxy group number ag galactic absorption in B-mag according to RC2 ai internal absorption (in B-mag) incl inclination (angle between line of sight and polar axis) a21 HI self-absorption lambda luminosity-index according to G. de Vaucouleurs logdc log10 of the corrected diameter (dc in 0.1') btc corrected B-magnitude ubtc (U-B)o bvtc (B-V)o bri25 mean surface brightness within 25 m/" (mag.arcsec-2) logvm log10 of maximum circular rotation velocity (corrected for incl) m21c corrected HI-magnitude (corrected for a21) hic HI color index vlg radial velocity relative to the Local Group centroid vgsr radial velocity relative to the galactic Std. of rest vvir radial velocity corrected for velocity infall on Virgo v3k radial velocity relative to the 3K background radiation mucin kinematical distance modulus (H=75 km/s/Mpc) mupar photometric distance modulus mabs absolute B magnitude from mucin and mupar For the selection: select pgc,ident1,al2000,de2000,bt where (bt+5*logd25)<20 end The output will looks like (just an extract!) : Conditions for extraction : [[bt + [5 * logd25]] < 20] pgc ident1 al2000 de2000 bt PGC 000006 CGCG 456- 13 0.0006 15.8814 15.3900 PGC 000007 MCG 0- 1- 14 0.0012 -0.0830 15.4200 PGC 000009 ESO 12- 11A 0.0021 -77.3376 17.3800 PGC 000010 MCG 0- 1- 15 0.0022 -0.0405 15.4900 PGC 000011 ESO 12- 11 0.0023 -77.3399 16.9000 PGC 000005 IC 5370 0.0025 32.7389 14.8900 PGC 000020 MCG 0- 1- 16 0.0044 1.1450 15.1600 PGC 000027 MCG -1- 1- 18 0.0060 -6.9049 14.5000 Note that all pieces of information extracted from the SQL-like option are stored in a single file. Thus, avoid to make several long queries in a single session. BATCH MODE ========== If you want to make a study (e.g. extract data, charts, plot on a Flamsteed projection) from a list of galaxy names or galaxy positions, it is not necessary to keypunch these names or positions in an on-line connection. Just send your list of galaxy identifiers to: LEDAMAIL@LMC.UNIV-LYON1.FR You will receive in reply to your mail a file with the result. Give as a Subject of the mail one of the following keywords, and follow the instruction for the format to use in your mail. Subject: LIST -------------- You will receive in reply to your mail a file with the main parameters needed for good identification of the galaxies of your list. These parameters are: coordinates, alternative names, apparent diameter and axis ratio, apparent magnitude, radial velocity. FORMAT OF YOUR MAIL : one identifier per line (Name or 1950-RA.DEC in free format). EXAMPLE: NGC598 121921.4+044458 UGC3615 n224 Subject: LISTALL ---------------- You will receive a file with all astrophysical parameters for your galaxies. The format of this file is given in 'ANNEX A' below. FORMAT OF YOUR MAIL : one identifier (Name or 1950-RA.DEC) per line. EXAMPLE: ESO122.12 12h19m21.4s 4d44'58" UGC5005 Subject: FLAMEQ (or FLAMGA or FLAMSG) -------------------------------------- You will receive a postscript file with an all-sky Flamsteed equal-area projection of your objects in either equatorial or galactic or supergalactic coordinates, depending on the Subject you selected. To print this file just send it to a laser printer with postscript language. FORMAT OF YOUR MAIL : one identifier (Name or 1950-RA.DEC) per line. EXAMPLE: LMC 121921.4+044458 UGC4612 Subject: CHART -------------- You will receive a postscript file with charts (max 20), and a corresponding file with data. FORMAT OF YOUR MAIL : -one line with an identifier (Name or 1950-RA.DEC) -one line with the radius in arcmin (0=PSS or ESO scale) EXAMPLE: me31 0 12 19 21.4 4 44 58 100 (this will create two charts (in one file) : the first one centered on Messier 31 with the PSS scale. the second one will create a chart centered on the position RA1950=12h19m21.4s DEC1950=04d44'58" with a 100' radius) Subject: SQL ------------ The principle consists in giving a sentence which describes the request. You will receive a file corresponding to the result of you request. See the instructions for use to learn how to use it, and to know the name and the description of the parameters. FORMAT OF YOUR MAIL : only one line per selection and one selection per mail. EXAMPLE: select ident1,logd25 where (w20>200 and w20<300) end Good luck! If you are satisfied using LEDA, we would appreciate your quoting LEDA in publications you derive from it. This will encourage us to pursue our efforts. Thank you. G. Paturel LEDA Lyon-Meudon Extragalactic Database Observatoire de Lyon 69561 Saint-Genis Laval CEDEX, France patu@lmc.univ-lyon1.fr ACKNOWLEDGEMENTS: ================= This database has been developed with the help of many people, Becker M., Bottinelli L., Buta R.J., Corwin H.G.Jr., Davoust E., de Vaucouleurs A., de Vaucouleurs G., Durand N., Fouque P., Garnier R., Kogoshvili N., Gouguenheim L., Hallet N., Marthinet M.C., Miyauchi-Isobe N., Odewahn S., Petit C., Prugniel Ph., Andernach H., Simien F., Takase B., Mamon G. and the following Institutions INSU, CNRS, DRED, Conseil Regional Rhone-Alpes, Observatoire de Lyon, Observatoire de Paris-Meudon, Centre de Donnees Stellaires de Strasbourg. ANNEX A: FORMAT OF THE FILE BUILD FROM THE 'LISTALL' OPTION =========================================================== NAME FORMAT COLUMNS NOTE ========================================================= Name a20,1x 1 - 21 Name as given by user al1950 f8.5 21 - 28 de1950 f8.4 29 - 36 ipad 1x,a1,1x 37 - 39 al2000 f8.5 40 - 47 de2000 f8.4 48 - 55 l2 f6.2 56 - 61 b2 f6.2 62 - 67 sgl f6.2 68 - 73 sgb f6.2 74 - 79 pgc a10 80 - 89 ident1 a16 90 - 106 pa f6.1 107 - 112 typ a5 113 - 117 ring a1 118 - 118 multiple a1 119 - 119 compact a1 120 - 120 t f6.1 121 - 126 st f6.1 127 - 132 lc f6.1 133 - 138 slc f6.1 139 - 144 logd25 f6.2 145 - 150 slogd25 f6.2 151 - 156 logr25 f6.2 157 - 162 slogr25 f6.2 163 - 168 brief f6.2 169 - 174 sbrief f6.2 175 - 180 bt f6.2 181 - 186 sbt f6.2 187 - 192 ubt f6.2 193 - 198 bvt f6.2 199 - 204 ube f6.2 205 - 210 bve f6.2 211 - 216 w20 i6 217 - 222 sw20 i6 223 - 228 w50 i6 229 - 234 sw50 i6 235 - 240 logs f6.3 241 - 246 slogs f6.3 247 - 252 m21 f6.2 253 - 258 sm21 f6.2 259 - 264 mfir f6.2 265 - 270 vrad i6 271 - 276 svrad i6 277 - 282 vopt i6 283 - 288 svopt i6 289 - 294 v i6 295 - 300 sv i6 301 - 306 lgg i6 307 - 312 ag f6.2 313 - 318 ai f6.2 319 - 324 incl f6.1 325 - 330 a21 f6.2 331 - 336 lambda f6.2 337 - 342 logdc f6.2 343 - 348 btc f6.2 349 - 354 ubtc f6.2 355 - 360 bvtc f6.2 361 - 366 bri25 f6.2 367 - 372 logvm f6.3 373 - 378 m21c f6.2 379 - 384 hic f6.2 385 - 390 vlg i6 391 - 396 vgsr i6 397 - 402 vvir i6 403 - 408 v3k i6 409 - 414 mucin f6.2 415 - 420 mupar f6.2 421 - 426 mabs f6.2 427 - 432 ANNEX B: DEFINITION AND CALCULATION OF ASTROPHYSICAL PARAMETERS =============================================================== al1950, de1950 1950 right ascension and declination in decimal hours and degres, respectively ipad flag to tell that al,de are accurate (*=accurate) accurate means better than 10" al2000, de2000 2000 right ascension and declination in decimal hours and degres, respectively l2, b2 galactic longitude and latitude in degres sgl, sgb supergalactic longitude and latitude in degres (pole and origin conforms to the RC2 reference system) pgc/leda LEDA identifier (PGC number when it exists) ident1 Alternative name given according to a hierarchy NGC; IC; UGC; ESO; MCG; UGCA; MARK; DDO; CGCG; FAIR; ARAK; UM; ZW;1 KUG; HICK; VCC; IRAS; WEIN; VIII; ISZ; POX; KAZA; KARA; CR; RB; DRCG; SAIT; KCPG; FGC; FGCE; FGCA; For the description of names see Paturel et al. 1989a, 1989b pa position angle (in degres measured from North towards Est) typ mean morphological type ring 'R' for Ring galaxies, otherwise ' ' (blank) multiple 'M' for multiple galaxies, otherwise ' ' (blank) compact 'C' for compact, 'D' for diffuse, otherwise ' ' t mean morphological type code according to RC3 (de Vaucouleurs et al. 1992) (E=-5 ; SO=-2 ; Sa=1 ; Sb=3 ; Sc=6 ; Sm=9 ; Irr=10) st mean error on typ code lc luminosity class coded according to RC3 (I=1 ; I-II=2 ; II=3 ...) slc mean error on luminosity class logd25 log of the apparent major axis of the galaxy at the 25 mag.arsec-2 surface brightness level. d25 is in 0.1'. slogd25 mean error on logd25 logr25 logr25=log(d25/b25) where d25 and b25 are major and minor axes, respectively slogr25 mean error on logr25 The last four quantitites are calculated according to Paturel et al. 1991. brief mean effective surface brightness in B. The definition is the one given in the RC3 catalog but it is expressed in mag.arcsec-2. (bt+0.753) + 5logde -5.26 + 8.891, where bt is the total B magnitude, and de the effective diameter in 0.1'. sbrief mean error on brief bt total (or asymptotic) blue magnitude sbt mean error on bt The last two quantities are derived from Paturel et al. 1993 (submitted). ubt total (U-B) color from aperture photoelectric photometry bvt total (B-V) color from aperture photoelectric photometry ube mean effective (U-B) color from aperture photoelectric photometry bve mean effective (B-V) color from aperture photoelectric photometry The definition of the last four quantities is taken according to the RC3 w20 mean 21-cm line width at 20% of the maximum (in km/s) sw20 mean error on w20 (in km/s) w50 mean 21-cm line width at 50% of the maximum (in km/s) sw50 mean error on w50 (in km/s) The last four quantities are calculated according to Bottinelli et al. 1990. They are corrected only for instrumental resolution effect. logs decimal log of the central velocity dispersion (in km/s) slogs mean error on logs m21 magnitude corresponding to the 21-cm line area. The definition of m21 conforms to the RC3 definition: m21= 16.6 - 2.5logSH where SH is expressed in 10-22 W.m-2 m21 is corrected for beam filling effect and is calculated according to Bottinelli et al. 1990. sm21 mean error on m21 mfir far-infrared magnitude derived from the IRAS point source Catalog. The definition is the following: amfir=-20 -2.5log(FIR) where FIR=1.26 [2.58f(60) + f(100)]x10-14 f(60) and f(100) being the IRAS fluxes at 60 and 100 micron respectively. FIR is expressed in W.m-2. vrad mean heliocentric radial velocity from 21-cm line measurements in km/s. svrad mean error on vrad The last two quantities are derived according to Bottinelli et al. 1990 vopt heliocentric mean radial velocity from optical measurement. svopt mean error on vopt The last two quantitites are derived according to Fouque et al. 1992 v mean heliocentric velocity in km/s (weighted mean of vrad and vopt). The weights are calculated as the inverse of the square of the mean error. sv mean error on vm. lgg Lyon's galaxy group number (LGG) according to Garcia 1993 ag galactic absorption in blue magnitude. This absorption is calculated according to the RC2. ai total internal absorption in blue magnitude It is calculated according to Tully and Fouque 1985 incl inclination between the line of sight and the polar axis of the galaxy. It is calculated from axis ratio through the ellipsoidal model: sini= sqrt((1-q2)/(1-qo2)) where q=d25/D25 and qo is given as a function of morphological type code qo=.43+0.053t and qo=0.38 for t>7 (Fouque, private communication) a21 HI self-absorption according to Heidmann et al. (1971) with coef. tau=0.031 lambda luminosity index corrected for inclination effect. This index has been defined by G. de Vaucouleurs 1979 as: Lambda-c=(T+Lv)/10 where T is the morphological type code and Lc the luminosity class corrected for inclination effect. logdc decimal log of the corrected apparent diameter Do, where Do is in 0.1'. logDo is corrected for galactic absorption and inclination effect using the following relation: logDo=logD25 - 0.235logR25 +ag(0.081-0.016T) btc corrected total apparent blue magnitude Bo corrected for galactic absorption, internal absorption and redshift effect The corrected magnitude is calculated using the relation: btc= bt - ag -ai -K.v where v is the heliocentric radial velocity and K a function of morphological type code t (according to RC2) ubtc (U-B)T color, corrected according to RC2 bvtc (B-V)T color, corrected according to RC2 bri25 mean surface brightness at the 25 mag.arcsec-2 surface brightness level. This mean surface brightness is expressed in mag. arcsec-2. logvm log of the maximum velocity rotation Vm from 21-cm line width w20 and w50. Vm is corrected for inclination effect and for internal dispersion according to Tully and Fouque 1985 m21c corrected HI magnitude m21c. A correction of self-absorption is made according to Heidmann et al. 1971 hic hydrogen index HI defined following: hic=m21c-btc vlg mean radial velocity in km/s corrected for solar motion towards the centroid of the Local Group. The correction is made according to Yahil et al. 1977 vgsr radial velocity in km/s, corrected for solar motion toward the galactic standard of rest. The correction is made according to RC3. (232.3 km/s toward l2=87.8d b2=1.7d) vvir radial velocity in km/s, corrected for infall of the Local Group toward the Virgo cluster. The adopted infall velocity is 150 km/s toward supergalactic position sgl=104 degres, sgb=-2 degres (Virgo center) v3k radial velocity in km/s, corrected to the reference frame of the 3K radiation according to Lubin and Villela 1986. (solar motion 360 km/s toward al1950=11.25h de1950=-5.6deg) mucin distance modulus calculated from kinematical velocity vvir using a Hubble constant of 75 (km/s)/Mpc. The distance modulus is not calculated for vvir<500 km/s. mupar mean distance modulus calculated from parameters using a weighted mean of all distance criteria (logVm, Lambda-c, dispv, U-B). The adopted relation are the following: amu=bt0+6.5*alvm+6.3+0.02*vm/1000. amu=bt0-3.4*alac+22.9+0.16*vm/1000. amu=bt0+6.2*dispv+5.9+0.16*vm/1000 amu=bt0+4.4*umb0+17.8+0.26*vm/1000 The vm correction aims at correcting for Malmquist bias. Obviously such a correction is only a tentative improvement. mabs absolute magnitude derived from the adopted distance modulus mucin and corrected apparent magnitude btc. REFERENCES ---------- - Bottinelli, L., Gouguenheim,L., Fouque, P., Paturel, G., 1990 A&AS 82, 391 - de Vaucouleurs G., Vaucouleurs A., Corwin, H.G. Jr, 1976, Second Reference Catalogue of Bright Galaxies, Texas University Press, Austin (RC2) - de Vaucouleurs G., 1979, ApJ. 227, 380 - de Vaucouleurs, A., de Vaucouleurs, G., Corwin, H.G.Jr, Buta, R.J., Paturel, G., Fouque, P. 1991 ed. Springer-Verlag New-York Inc. (RC3) - Fouque, P., Durand, N., Bottinelli, L. ,Gouguenheim, L., Paturel, G., 1992, Monographies de la base de donnees extragalactiques, No.3 , Lyon (ISBN 2.908288.05.2) - Garcia A.M., 1993, A&AS 100, 47 - Heidmann, Heidmann, de Vaucouleurs, 1971, MemRAS 75, 85 - Paturel,G., Fouque,P., Buta, R.J., Garcia, A.M., 1991, A&A 243, 319 - Paturel G., Fouque P., Bottinelli L., Gouguenheim L., 1989a, A&AS 80,209 - Paturel G., Fouque P., Bottinelli L., Gouguenheim L., 1989b, Principal Galaxy Catalog, Monographies de la base de donnees extragalactiques, No.1 , Lyon (ISBN 2.908288.00.1) (PGC) - Tully, R., Fouque, P., 1985, ApJS 58,67 - Lubin P., Villela T., 1986, in Galaxy Distances and Deviations from Universal Expansion, ed. B.F. Madore and R.B. Tully, Dordrecht: Reidel, p169 - Yahil, A, Tammann, G.,A., Sandage, A., 1977, ApJ 217, 903