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 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 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:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
catalog.dat 632 5859 Emission line catalog
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See also:
J/A+A/566/A32 : Equivalent widths of WINGS galaxies (Fritz+, 2014)
Byte-by-byte Description of file: catalog.dat
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Bytes Format Units Label Explanations
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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 A11.6 --- 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)
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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
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Acknowledgements:
Paola Marziani, paola.marziani(at)oapd.inaf.it
(End) Paola Marziani [INAF, Italy], Patricia Vannier [CDS] 04-Nov-2016