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J/A+A/599/A83       ELG and AGN in WINGS clusters            (Marziani+, 2017)

Emission line galaxies and active galactic nuclei in WINGS clusters. Marziani P., D'Onofrio M., Bettoni D., Poggianti B.M., Moretti A. Fasano G., Fritz J., Cava A., Varela J., Omizzolo A. <Astron. Astrophys. 599, A83 (2017)> =2017A&A...599A..83M (SIMBAD/NED BibCode)
ADC_Keywords: Clusters, galaxy ; Galaxy catalogs ; Spectroscopy Keywords: catalogs - galaxies: clusters: general - galaxies: clusters: intracluster medium - galaxies: star formation - galaxies: statistics - galaxies: evolution Abstract: We present the analysis of the emission line galaxies members of 46 low-redshift (0.04<z<0.07) clusters observed by WINGS (WIde-field Nearby Galaxy cluster Survey; Fasano et al., 2006A&A...445..805F). Emission line galaxies were identified following criteria that are meant to minimize biases against non-star-forming galaxies and classified employing diagnostic diagrams. We examined the emission line properties and frequencies of star-forming galaxies, transition objects, and active galactic nuclei (AGNs: LINERs and Seyferts), unclassified galaxies with emission lines, and quiescent galaxies with no detectable line emission. A deficit of emission line galaxies in the cluster environment is indicated by both a lower frequency, and a systematically lower Balmer emission line equivalent width and luminosity with respect to control samples; this implies a lower amount of ionized gas per unit mass and a lower star formation rate if the source is classified as Hii region. A sizable population of transition objects and of low-luminosity LINERs (∼10-20% of all emission line galaxies) are detected among WINGS cluster galaxies. These sources are a factor of 1.5 more frequent, or at least as frequent, as in control samples with respect to Hii sources. Transition objects and LINERs in clusters are most affected in terms of line equivalent width by the environment and appear predominantly consistent with so-called retired galaxies. Shock heating can be a possible gas excitation mechanism that is able to account for observed line ratios. Specific to the cluster environment, we suggest interaction between atomic and molecular gas and the intracluster medium as a possible physical cause of line-emitting shocks. Description: Emission line parameters for 5859 galaxies in the central regions of 46 ROSAT clusters are presented. Galaxies in the following clusters have been observed: A1069 A119 A151 A1631a A1644 A1831 A193 A1983 A1991 A2107 A2124 A2169 A2382 A2399 A2415 A2457 A2572a A2589 A2593 A2622 A2626 A3128 A3158 A3266 A3376 A3395 A3490 A3497 A3556 A3560 A376 A3809 A500 A671 A754 A957x A970 IIZW108 MKW3s RX0058 RX1022 RX1740 Z2844 Z8338 Z8852 For each galaxy we report cluster membership, rest-frame equivalent width of Hbeta and Halpha, errors or censorship flags, diagnostic ratios with errors or censorship flag, probability of correct classification from the location in the diagnostic diagrams (DDs), fluxes derived from photometry, log of luminosity, and notes. The identification of 7 Seyfert 1s is reported in the notes. See Section 4.1 of the paper for a more detailed explanation. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file catalog.dat 632 5859 Emission line catalog
See also: J/A+A/566/A32 : Equivalent widths of WINGS galaxies (Fritz+, 2014) Byte-by-byte Description of file: catalog.dat
Bytes Format Units Label Explanations
1- 5 A5 --- --- [WINGS] 6- 24 A19 --- WINGS WINGS identifier (JHHMMSS.ss+DDMMSS.s) 26- 32 A7 --- Cluster Cluster identification code 34 I1 --- Memb [0/1] Membership (1) 36- 48 A13 --- IDS Id with spectrum aperture number 50- 57 F8.3 --- SN 1-sigma S/N ratio close to [OIII] 59- 66 F8.3 --- ROII ?=-999 Ratio[OII]/rms[OII] 68- 75 F8.3 --- RHB ?=-999 Ratio Hbeta/rmsHbeta (6) 77- 84 F8.3 --- ROIII ?=-999 Ratio [OIII]/rms[OIII] (6) 86- 93 F8.3 --- ROI ?=-999 Ratio [OI]/rms[OI] (6) 95-102 F8.3 --- RHa ?=-999 Ratio Halpha/rmsHalpha (6) 104-111 F8.3 --- RNII ?=-999 Ratio [NII]/rms[NII] (6) 113-123 F11.3 --- RSII ?=-999 Ratio [SII]/rms[SII] (6) 125 I1 --- Detect [0/1] Detection of emission lines following criterion of Eq. 2 127-133 F7.3 0.1nm EWMin Minimum eq. width detectable at reported S/N, from Eq. A.1 135-142 F8.3 0.1nm EWHb ?=-999 Rest-frame EW of Hbeta (6) 144-151 F8.3 0.1nm e_EWHb ?=-999 Hbeta EW error 153-156 I4 --- f_EWHb [-1/1]? Hbeta EW censorship (2) 158-165 F8.3 0.1nm EWHa ?=-999 Rest-frame Halpha EW (6) 167-174 F8.3 0.1nm e_EWHa ?=-999 Halpha EW error 176-181 F6.1 --- f_EWHa [-1/0]? Halpha EW censorship (2) 183-190 F8.3 --- ROIIHB ?=-999 Log_10 [OII]/Hbeta (6) 192-199 F8.3 --- e_ROIIHB ?=-999 Lower error on Log[OII]/Hbeta 201-208 F8.3 --- E_ROIIHB ?=-999 Upper error on Log[OII]/Hbeta 210-213 I4 --- f_ROIIHB [-1/1]? Log[OII]/Hbeta censorship (2) 215-222 F8.3 --- ROIIIHB ?=-999 Log_10 [OIII]/Hbeta (6) 224-231 F8.3 --- e_ROIIIHB ?=-999 Lower error on Log[OIII]/Hbeta 233-240 F8.3 --- E_ROIIIHB ?=-999 Upper error on Log[OIII]/Hbeta 242-245 I4 --- f_ROIIIHB [-1/1]? Log[OIII]/Hbeta censorship (2) 247-254 F8.3 --- ROIHa ?=-999 Log_10 [OI]/Halpha (6) 256-263 F8.3 --- e_ROIHa ?=-999 Lower error on Log[OI]/Halpha 265-272 F8.3 --- E_ROIHa ?=-999 Upper error on Log[OI]/Halpha 274-277 I4 --- f_ROIHa [-1/1]? Log[OI]/Halpha censorship (2) 279-286 F8.3 --- RNIIHa ?=-999 Log_10 [NII]/Halpha (6) 288-295 F8.3 --- e_RNIIHa ?=-999 Lower error on Log [NII]/Halpha 297-304 F8.3 --- E_RNIIHa ?=-999 Upper error on Log [NII]/Halpha 306-309 I4 --- f_RNIIHa [-1/1]? Log[NII]/Halpha censorship (2) 311-318 F8.3 --- RSIIHa ?=-999 Log_10 [SII]/Halpha (6) 320-327 F8.3 --- e_RSIIHa ?=-999 Lower error on Log [SII]/Halpha 329-336 F8.3 --- E_RSIIHa ?=-999 Upper error on Log [SII]/Halpha 338-341 I4 --- f_RSIIHa [-1/1]? Log[SII]/Halpha censorship (2) 343-344 A2 --- ClassOII Class from [OII] DD (3) 346-354 E9.6 --- POIIHII ?=-999 HII probability in [OII] DD 356-365 E10.6 --- POIILIN ?=-999 LINER probability in [OII] DD 367-376 E10.6 --- POIISeyf ?=-999 Seyfert probability in [OII] DD 378-379 A2 --- ClassOIIRev Revised class from [OII] DD (3) 381-382 A2 --- ClassOI Class from [OI] DD (3) 384-385 A2 --- ClassNII Class from [NII] DD (4) 387-396 E10.6 --- PNIIHII ?=-999 Probability of HII in [NII] DD 398-407 E10.6 --- PNIITO ?=-999 Probability of TO in [NII] DD 409-419 A11 --- PNIILIN ?=-999 Probability of LINER in [NII] DD 421-430 E10.6 --- PNIISeyf ?=-999 Seyfert probability in [NII] DD 432-433 A2 --- ClassNIIRev Revised class from [NII] DD (4) 435-436 A2 --- ClassSII Class from [SII] DD (3) 438-446 E9.4 10-2W/m2/nm FL ? Specific flux at 5000 448-456 E9.4 10-2W/m2/nm FLV ? Specific flux from V-band 458-465 F8.3 10-7W logLHb ? Log_10 Hbeta emission line luminosity 467-470 I4 --- f_logLHb [-1/1]? Hbeta luminosity censorship (2) 472-479 F8.3 10-7W logLHa ? Log_10 Halpha emission line luminosity 481-484 I4 --- f_logLHa [-1/1]? Halpha luminosity censorship (2) 486-632 A147 --- Notes Notes on individual sources(5)
Note (1): Membership code: 1 = cluster member 0 = non-member Note (2): Censorship flag as follows: -1 = upper limit 1 = lower limit 0 = detection Note (3): Class code as follow: U = emission lines undetected E = emission lines detected but no classification from DD EH = HII EL = LINER ES = Seyfert Note (4): Class code as follow: U = emission lines undetected E = emission lines detected but no classification from DD EH = HII EL = LINER ES = Seyfert ET = transition objects (TOs) Note (5): Technical notes; identification of possible Seyfert candidates along with seven Seyfert 1s that have been identified: WINGSJ012442.24+085124.4 WINGSJ034144.52-534221.1 (S1.9) WINGSJ042931.90-613820.0 WINGSJ043838.78-220325.0 WINGSJ060131.87-401646.9 WINGSJ125732.47-173633.1 WINGSJ132513.37-313137.7. Note (6): Errors codes: -999 = unavailable -888 = line intensity ratio cannot be computed because both lines are censored
Acknowledgements: Paola Marziani, paola.marziani(at)oapd.inaf.it
(End) Paola Marziani [INAF, Italy], Patricia Vannier [CDS] 04-Nov-2016
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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