J/AJ/124/2453 Spectroscopy of active galaxies in nearby clusters (Miller+, 2002) ================================================================================ Evolution of star-forming and active galaxies in nearby clusters. Miller N.A., Owen F.N. =2002AJ....124.2453M ================================================================================ ADC_Keywords: Clusters, galaxy ; Radio continuum ; Galaxies, spectra Keywords: galaxies: clusters: general - galaxies: evolution - radio continuum Abstract: We have used optical spectroscopy to investigate the active galaxy populations in a sample of 20 nearby Abell clusters. The targets were identified on the basis of 1.4GHz radio emission, which identifies them as either active galactic nuclei (AGNs) or galaxies forming stars at rates comparable to or greater than that of the Milky Way. The spectra were used to characterize the galaxies via their emission and absorption features. File Summary: -------------------------------------------------------------------------------- FileName Lrecl Records Explanations -------------------------------------------------------------------------------- ReadMe 80 . This file table3.dat 78 619 D_4000_ and Balmer equivalent widths for cluster radio galaxies table4.dat 96 619 Forbidden-line equivalent widths for cluster radio galaxies table5.dat 73 236 Balmer line fluxes for cluster radio galaxies table6.dat 94 234 Forbidden-line fluxes for cluster radio galaxies table8.dat 39 229 Galaxy classifications -------------------------------------------------------------------------------- See also: J/ApJS/134/355 : Radio galaxies in 18 nearby Abell clusters (Miller+, 2001) Byte-by-byte Description of file: table3.dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 1- 13 A13 --- [MO2002] Galaxy identification (G1) 15 A1 --- Apt Extraction aperture (G2) 17- 20 F4.2 --- D4000 ? The 4000{AA} break strength (2) 22- 25 F4.2 --- e_D4000 ? Error in D4000 27- 31 F5.1 0.1nm EWHd H{delta} equivalent width in {AA} (3) 33- 36 F4.1 0.1nm e_EWHd Error in EWHd 38- 41 F4.1 0.1nm EWHg H{gamma} equivalent width in {AA} (3) 43- 46 F4.1 0.1nm e_EWHg Error in EWHg 48- 51 F4.1 0.1nm EWHb H{beta} equivalent width in {AA} (3) 53- 55 F3.1 0.1nm e_EWHb Error in EWHb 57- 61 F5.1 0.1nm EWHa+NII H{alpha}+[N II] equivalent width in {AA} (3) 63- 66 F4.1 0.1nm e_EWHa+NII Error in EWHa+NII 68- 72 F5.1 0.1nm EWHa ? H{alpha} equivalent width in {AA} (3) 74- 77 F4.1 0.1nm e_EWHa ? Error in EWHa -------------------------------------------------------------------------------- Note (2): The ratio of average F_{nu}_ evaluated in the ranges 4050-4250{AA} to 3750-3950{AA} (Bruzual, 1983ApJ...273..105B). Note (3): With the exception of H{alpha} + [N II], these equivalent widths have been corrected for the assumed Balmer absorption component caused by starlight in the galaxies. The adopted convention has positive equivalent widths representing emission lines and negative equivalent widths representing absorption. Where blends occur, the deblending has been performed in IRAF using the task SPLOT as described in the text. -------------------------------------------------------------------------------- Byte-by-byte Description of file: table4.dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 1- 13 A13 --- [MO2002] Galaxy identification (G1) 15 A1 --- Apt Extraction aperture (G2) 17- 21 F5.1 0.1nm EWOII ? The [O II] {lambda}3727 equivalent width (2) 23- 26 F4.1 0.1nm e_EWOII ? Error in EWOII 28- 31 F4.1 0.1nm EWO4959 The [O III] {lambda}4959 equivalent width (2) 33- 35 F3.1 0.1nm e_EWO4959 Error in EWO4959 37- 40 F4.1 0.1nm EWO5007 The [O III] {lambda}5007 equivalent width (2) 42- 44 F3.1 0.1nm e_EWO5007 Error in EWO5007 46- 49 F4.1 0.1nm EWOI The [O I] {lambda}6300 equivalent width (2) 51- 54 F4.1 0.1nm e_EWOI Error in EWOI 56- 60 F5.1 0.1nm EWNII ? The [N II] {lambda}6584 equivalent width (2) 62- 65 F4.1 0.1nm e_EWNII ? Error in EWNII 67- 70 F4.1 0.1nm EWSII ? The [S II] doublet equivalent width (2) 72- 75 F4.1 0.1nm e_EWSII ? Error in EWSII 77- 80 F4.1 0.1nm EWS6717 ? The [S II] {lambda}6717 equivalent width (2) 82- 85 F4.1 0.1nm e_EWS6717 ? Error in EWS6717 87- 90 F4.1 0.1nm EWS6731 ? The [S II] {lambda}6731 equivalent width (2) 92- 95 F4.1 0.1nm e_EWS6731 ? Error in EWS6731 -------------------------------------------------------------------------------- Note (2): The adopted convention has positive equivalent widths representing emission lines and negative equivalent widths representing absorption. Where blends occur, the deblending has been performed in IRAF using the task SPLOT as described in the text. -------------------------------------------------------------------------------- Byte-by-byte Description of file: table5.dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 1- 13 A13 --- [MO2002] Galaxy identification (G1) 15 A1 --- Apt Extraction aperture (G2) 17- 21 F5.2 10-15mW/m2 FHd H{delta} flux (in 10^-15^erg/s/cm^2^) (2) 23- 26 F4.2 10-15mW/m2 e_FHd Error in FHd (3) 28- 32 F5.2 10-15mW/m2 FHg H{gamma} flux (in 10^-15^erg/s/cm^2^) (2) 34- 37 F4.2 10-15mW/m2 e_FHg Error in FHg (3) 39- 43 F5.2 10-15mW/m2 FHb H{beta} flux (in 10^-15^erg/s/cm^2^)(2) 45- 48 F4.2 10-15mW/m2 e_FHb Error in FHb (3) 50- 55 F6.2 10-15mW/m2 FHa+NII H{alpha}+[N II] flux (in 10^-15^erg/s/cm^2^) (2) 57- 60 F4.2 10-15mW/m2 e_FHa+NII Error in FHa+NII (3) 62- 67 F6.2 10-15mW/m2 FHa H{alpha} flux (in 10^-15^ ergs/s/cm^2^) (2) 69- 72 F4.2 10-15mW/m2 e_FHa Error in FHa (3) -------------------------------------------------------------------------------- Note (2): Only galaxies with emission lines are presented in this table. Values of 0.00 indicate that the line was not detected in emission. Where blends occur, the deblending has been performed in IRAF using the task SPLOT as described in the text. Note (3): Errors are based on the error in the continuum around the line, bootstrapped to the line region taking into account the relative sizes of the line and continuum regions. For deblended lines, a line extraction region of 20{AA} was assumed. -------------------------------------------------------------------------------- Byte-by-byte Description of file: table6.dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 1- 13 A13 --- [MO2002] Galaxy identification (G1) 15 A1 --- Apt Extraction aperture (G2) 17- 22 F6.2 10-15mW/m2 FlOII The [O II] {lambda}3727 flux (in 10^-15^erg/s/cm^2^) (2) 24- 27 F4.2 10-15mW/m2 e_FlOII Error in FlOII (3) 29- 33 F5.2 10-15mW/m2 FlO4959 The [O III] {lambda}4959 flux (in 10^-15^erg/s/cm^2^) (2) 35- 38 F4.2 10-15mW/m2 e_FlO4959 Error in FlO4959 (3) 40- 44 F5.2 10-15mW/m2 FlO5007 The [O III] {lambda}5007 flux (in 10^-15^erg/s/cm^2^) (2) 46- 49 F4.2 10-15mW/m2 e_FlO5007 Error in FlO5007 (3) 51- 55 F5.2 10-15mW/m2 FlOI The [O I] {lambda}6300 flux (in 10^-15^erg/s/cm^2^) (2) 57- 60 F4.2 10-15mW/m2 e_FlOI Error in FlOI (3) 62- 66 F5.2 10-15mW/m2 FlNII The [N II] {lambda}6584 flux (in 10^-15^erg/s/cm^2^) (2) 68- 71 F4.2 10-15mW/m2 e_FlNII Error in FlNII (3) 73- 77 F5.2 10-15mW/m2 FlS6717 The [S II] {lambda}6717 flux (in 10^-15^erg/s/cm^2^) (2) 79- 82 F4.2 10-15mW/m2 e_FlS6717 Error in FlS6717 (3) 84- 88 F5.2 10-15mW/m2 FlS6731 The [S II] {lambda}6731 flux (in 10^-15^erg/s/cm^2^) (2) 90- 93 F4.2 10-15mW/m2 e_FlS6731 Error in FlS6731 (3) -------------------------------------------------------------------------------- Note (2): Only galaxies with emission lines are presented in this table. Values of 0.00 indicate that the line was not detected in emission. Where blends occur, the deblending has been performed in IRAF using the task SPLOT as described in the text. Note (3): Errors are based on the error in the continuum around the line, bootstrapped to the line region taking into account the relative sizes of the line and continuum regions. For deblended lines, a line extraction region of 20{AA} was assumed. -------------------------------------------------------------------------------- Byte-by-byte Description of file: table8.dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 1- 10 A10 --- CName Abell cluster name 12- 24 A13 --- [MO2002] Galaxy identification (G1) (1) 26- 28 A3 --- SpClass Spectral classification (2) 30- 33 A4 --- MORPHS MORPHS classification (3) 35 A1 --- f_MORPHS [ab] Flag on MORPHS (4) -------------------------------------------------------------------------------- Note (1): From J2000 coordinates. Note (2): Spectral classification: SF = star-forming galaxy; SF? = emission-line galaxy presumed to be star-forming, although line ratios are somewhat noisy; Abs = absorption-line spectrum with no apparent emission lines; Ab+ = predominantly absorption-line spectrum, although with slight emission of [N II] and sometimes [S II]; Sey = emission-line galaxy shown to be a Seyfert in line ratio tests; Lin = emission-line galaxy shown to be a LINER in line ratio tests; Mix = nuclear spectrum that of a Seyfert or LINER, with off-nuclear spectrum showing star formation. Note (3): Determined from full aperture spectrum. Table 7: MORPHs spectral classification scheme --------------------------------------------------------------------- Class [OII]{lambda}3727 H{delta} Comments EW in {AA} EW in {AA} --------------------------------------------------------------------- k Absent <3 Passive k+a Absent 3-8 Moderate Balmer absorption without emission a+k Absent >=8 Strong Balmer absorption without emission e(c) Yes, <40{AA} <4 Moderate Balmer absorption plus emission, spiral-like e(a) Yes >=4 Strong Balmer absorption plus emission e(b) Yes, >=40{AA} ... Starburst e(n) ... ... AGN from broad lines or [O III]{lambda}5007/H{beta} ratio --------------------------------------------------------------------- Adapted from Dressler et al., 1999, Cat. . The [O II] equivalent widths are for emission lines, and the H{delta} are for absorption lines. -------------------------------------------------------------------- Note (4): Flag on MORPHS classification: a: The [O II] line was not available in this spectrum. b: The wavelength coverage for the spectrum did not include the full blue continuum band for [O II], and hence no equivalent width or line flux is reported. However, the [O II] line is apparent in the spectrum. -------------------------------------------------------------------------------- Global notes: Note (G1): Nomenclature note: The identification names are HHMMSS+DDMMSS in the tables, and [MO2002] JHHMMSS+DDMMSS in Simbad Note (G2): Extraction aperture code: A: full 15" aperture; N: the 2" aperture; O: the difference between A and N. M: Denotes that the spectrum was obtained with the MX multifiber spectrometer and no spatial information can be obtained. Such spectra are not flux-calibrated, and consequently, meaningful values of D4000 cannot be calculated. For this reason, no correction for Balmer absorption has been applied to these spectra. Values are not presented in two cases: (1) all or some portion of the defined continuum region lay off the CCD, and (2) blended lines that were too weak to be deblended. -------------------------------------------------------------------------------- History: From electronic version of the journal Some modifications of name (from authors) on 09-Apr-2003 ================================================================================ (End) Greg Schwarz [AAS], Patricia Bauer [CDS] 13-Jan-2003