J/A+A/671/A118 SPRING catalogue (Cattorini+, 2023)
A complete spectroscopic catalogue of local galaxies in the northern spring sky.
Gas properties and nuclear activity in different environments.
Cattorini F., Gavazzi G., Boselli A., Fossati M.
<Astron. Astrophys. 671, A118 (2023)>
=2023A&A...671A.118C 2023A&A...671A.118C (SIMBAD/NED BibCode)
ADC_Keywords: Active gal. nuclei ; Equivalent widths ; Photometry, ultraviolet ;
Photometry, SDSS ; Redshifts ; H I data
Keywords: galaxies: active - galaxies: general - galaxies: interactions -
galaxies: evolution - galaxies: statistics - catalogs
Abstract:
With the aim of providing the complete demography of galaxies in the
local Universe, including their nuclear properties, we present SPRING,
a complete census of local galaxies limited to the spring quarter of
the Northern sky (10h<RA<16h; 0°<Dec<65°). The SPRING
catalogue is a flux- and volume-limited sample (r<17.7mag,
cz<10000km/s) of 30597 galaxies, including the Virgo, Coma and A1367
clusters. Images and spectra were individually examined to clear the
sample from unwanted entries. To inspect possible secular and
environmental dependencies of the various nuclear excitation
properties (SF vs. AGN), we perform a multidimensional analysis by
dividing the total sample according to (i) their position in the
(NUV-i) vs. Mstar diagram, (ii) local galaxy density, (iii)
stellar-mass, (iv) halo-mass of the group to which galaxies belong,
and (v) neutral Hydrogen content. We present a new calibration of the
optical diameter-based HI-deficiency parameter HIdef employing a
reference sample of isolated galaxies extracted from SPRING. At
intermediate distances between Virgo and Coma, we identify a ring-like
structure of galaxies constituted by three large filaments, each with
approximately 20h-1Mpc length, mostly composed of blue-cloud
galaxies with stellar-mass Mstar≲1010M☉. The fraction of
HI-deficient galaxies within the filament (30%) suggests that
filaments are a transitioning environment between field and cluster in
terms of HI content, as we find a clear progression from field
galaxies to filament and cluster galaxies for increasing HIdef
parameter. We classify the nuclear spectra according to the four-line
BPT and the two-line WHAN diagnostic diagrams, and investigate the
variation in the fraction of active nuclei hosts with stellar-mass, as
well as their colours and environments. We observe that the fraction
of LINERs is a steep function of stellar-mass, e.g., it is consistent
with zero up to Mstar≳109.5M☉ and becomes 40% for
Mstar≲1010.5M☉, whereas, for Mstar≲109-9:5M☉, almost
the entire spectroscopic sample is constituted of galaxies with
starforming nuclei. We investigate whether the nuclear-excitation
fractions depend predominantly on the stellar-mass or, conversely, on
the galaxy environment. In general, we observe that the
mass-dependency of the fraction of Seyfert nuclei is little sensitive
to the galaxy environment, whereas the fraction of star-forming nuclei
is a steeper function of stellar-mass in lower-density environments
and in blue-cloud galaxies. We find that the fraction of LINERs
depends on galaxy colour and, for Mstar≳109.510M☉, increases
in galaxies belonging to the green valley.
Description:
Table B1 (tableb1.dat) contains the SPRING catalogue described in the
paper. The SPRING catalogue is a complete census of local galaxies
limited to the Spring quarter of the North sky (10h<RA<16h;
0°<Dec<65°. It is a flux- and volume- limited sample of 30597
galaxies, including the Virgo, Coma, and A1367 clusters. Photometric
optical data are available for all entries. Petrosian (u,g,r,i,z)
magnitudes are taken from the SDSS. GALEX UV data are taken from the
catalogue by Voyer et al. 2014A&A...569A.124V 2014A&A...569A.124V, Cat. J/A+A/569/A124
(for Virgo galaxies) and from the Revised Catalog of GALEX Ultraviolet
Sources otherwise. Optical and UV data are corrected for Galactic
extinction and dust attenuation following the methods by Boselli et
al. (2014A&A...570A..69B 2014A&A...570A..69B, Cat. J/A+A/570/A69). Neutral Hydrogen (HI)
data are taken from the GoldMine database (Gavazzi et al.,
2003A&A...400..451G 2003A&A...400..451G), the Westerbork Coma Survey (Molnar et al.,
2022A&A...659A..94M 2022A&A...659A..94M, Cat. J/A+A/659/A94), the ALFALFA survey (Haynes
et al., 2011AJ....142..170H 2011AJ....142..170H, Cat. J/AJ/142/170; Durbala et al.,
2020AJ....160..271D 2020AJ....160..271D, Cat. J/AJ/160/271), and the HyperLEDA catalogue
(Makarov et al., 2014A&A...570A..13M 2014A&A...570A..13M). The adopted values of the
stellar-mass are calculated by the g and i corrected magnitudes
assuming a Chabrier IMF and following the prescription of Zibetti et
al., 2009MNRAS.400.1181Z 2009MNRAS.400.1181Z.. The local density around each object is
determined following the method of Gavazzi et al.
(2010A&A...517A..73G 2010A&A...517A..73G) in cylinders of 1Mpc radius and 1000km/s
half-length. The halo-mass is taken from the catalogue by Yang et al.
(2007ApJ...671..153Y 2007ApJ...671..153Y) and is determined from abundance matching
techniques between the halo-mass function and the stellar-mass (or
luminosity) of the most massive galaxy identified within the group.
For galaxies in the Virgo cluster (which are not present in Yang et
al., 2007ApJ...671..153Y 2007ApJ...671..153Y) we use the estimate reported by Boselli &
Gavazzi (2006PASP..118..517B 2006PASP..118..517B. Spectroscopic data are taken from the
SDSS emissionlinesport table (Thomas et al., 2013MNRAS.431.1383T 2013MNRAS.431.1383T) and
the Nasa-Sloan Atlas (Blanton et al., 2011AJ....142...31B 2011AJ....142...31B). Non-SDSS
spectra are taken from the updated Zwicky catalogue (Falco et al.,
1999PASP..111..438F 1999PASP..111..438F, Cat. J/PASP/111/438), the VCC catalogue (Binggeli
et al., 1985AJ.....90.1681B 1985AJ.....90.1681B, Cat. J/AJ/90/1681), the UGC catalogue
(Nilson, 1973, Cat. VII/26), the spectroscopic survey by Ho,
Filippenko, and Sargent (Ho et al., 1993, AASMA, 182, 17.05,
1995ApJS...98..477H 1995ApJS...98..477H, Cat. J/ApJS/98/477, 1997ApJS..112..315H 1997ApJS..112..315H, Cat.
J/ApJS/112/315), the survey taken by us with the Loiano 1.5m telescope
(Gavazzi et al., 2015A&A...580A.116G 2015A&A...580A.116G, this work), and spectra taken
with the MUSE IFU by Consolandi et al., 2017A&A...606A..83C 2017A&A...606A..83C; Fossati
et al., 2019MNRAS.484.2212F 2019MNRAS.484.2212F; Pedrini et al., 2022MNRAS.511.5180P 2022MNRAS.511.5180P.. We
provide nuclear-emission classification by optical spectra based on
the BPT (Baldwin et al., 1981PASP...93....5B 1981PASP...93....5B) and the WHAN (Cid
Fernandes et al., 2010MNRAS.403.1036C 2010MNRAS.403.1036C, 2011MNRAS.413.1687C 2011MNRAS.413.1687C)
diagnostics.
Table A1 (tablea1.dat) contains the spectroscopic data obtained by
G. Gavazzi and collaborators with the Loiano 1.5m telescope in the
years 2014-2020.
File Summary:
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FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
tablea1.dat 102 304 Loiano spectra (2014-2020)
tableb1.dat 140 30597 SPRING catalogue
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Byte-by-byte Description of file: tablea1.dat
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Bytes Format Units Label Explanations
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1- 19 A19 --- ID Galaxy name
21- 30 F10.6 deg RAdeg Right Ascension (J2000)
32- 40 F9.6 deg DEdeg Declination (J2000)
42- 46 I5 km/s cz Recessional velocity
48- 52 F5.2 mag rmag ?=- Observed r-band magnitude
54- 56 I3 s Tint Duration of the individual exposures
58 I1 --- N Number of individual exposures
60- 69 A10 "date" Obs.date Observing date
71- 73 I3 deg PAslit Slit orientation (counterclockwise from N);
270 corresponds to East-West
75- 81 F7.2 0.1nm EWHa Measured equivalent width of Halpha line
(negative EW values represent emission)
84- 89 F6.2 0.1nm EWNII Measured equivalent width of NII[6584] line
92- 96 F5.2 0.1nm EWHb ?=- Measured equivalent width of Hbeta line
98-102 F5.2 0.1nm EWOIII ?=- Measured equivalent width of OIII[5007]
line
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Byte-by-byte Description of file: tableb1.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 10 F10.6 deg RAdeg Right Ascension (J2000)
13- 21 F9.6 deg DEdeg Declination (J2000)
23- 27 F5.2 mag FUVcorr ?=- FUV magnitude corrected for
Galactic extinction and dust attenuation
29- 33 F5.2 mag NUVcorr ?=- NUV magnitude corrected for
Galactic extinction and dust attenuation
35- 39 F5.2 mag gmagcorr ?=- g-band magnitude corrected for
Galactic extinction and dust attenuation
41- 46 F6.3 mag imagcorr ?=- i-band magnitude corrected for
Galactic extinction and dust attenuation
47- 53 F7.1 km/s cz Recessional velocity
55- 60 F6.2 Mpc Dist Adopted distance in Mpc (H0=73km/s.Mpc)
62- 67 A6 --- Dbase Origin of the line measurement (1)
70- 78 F9.3 0.1nm EWHa ?=- Equivalent width of Halpha line
80- 87 F8.3 0.1nm EWNII ?=- Equivalent width of NII[6584] line
89- 96 F8.3 0.1nm EWHb ?=- Equivalent width of Hbeta line
98-106 F9.3 0.1nm EWOIII ?=- Equivalent width of OIII[5007] line
108-111 A4 --- BPT Adopted nuclear classification according
to the BPT diagram;
113-115 A3 --- WHAN Adopted nuclear classification according
to the WHAN diagram;
117-121 F5.2 [Msun] logMstar ?=- Adopted stellar-mass Log(Mstar)
calculated following Zibetti et al.,
2009MNRAS.400.1181Z 2009MNRAS.400.1181Z
123-128 F6.2 --- overdensity ?=- Local galaxy overdensity
130-134 F5.2 [Msun] logMhalo ?=- Halo mass Log(Mhalo)
136-140 F5.2 --- Hidef ?=- HI deficiency parameter
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Note (1): Origin of the line measurement code as follows:
SL = SDSS
HO = Ho et al. (1995ApJS...98..477H 1995ApJS...98..477H, Cat. J/ApJS/98/477,
1997ApJS..112..315H 1997ApJS..112..315H, Cat. J/ApJS/112/315)
ZW = Falco et al. (1999PASP..111..438F 1999PASP..111..438F, Cat. J/PASP/111/438)
LOI = Loiano (Gavazzi et al. 2011A&A...534A..31G 2011A&A...534A..31G, Cat. J/A+A/534/A31,
2013A&A...558A..68G 2013A&A...558A..68G, Cat. J/A+A/558/A68, this work)
NO = no nuclear spectrum available
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History:
From Federico Cattorini, fcattorini(at)uninsubria.it
Acknowledgements:
We are grateful to Paolo Franzetti and Alessandro Donati
for their contribution to GoldMine, the Galaxy On Line Database
(Gavazzi et al. 2003) extensively used in this work
(http://goldmine.mib.infn.it). We thank Andrea Maccio' for useful
discussion. We also thank the coordinator of the TAC, Giovannna Stirpe
for the generous time allocation at Loiano. This research has made use
of the NASA/IPAC Extragalactic Database (NED), which is operated by
the Jet Propulsion Laboratory, California Institute of Technology,
under contract with the National Aeronautics and Space Administration.
The present study made extensive use of SDSS. Funding for the Sloan
Digital Sky Survey (SDSS) and SDSS-II has been provided by the Alfred
P. Sloan Foundation, the Participating Institutions, the National
Science Foundation, the U.S. Department of Energy, the National
Aeronautics and Space Administration, the Japanese Monbukagakusho, and
the Max Planck Society, and the Higher Education Funding Council for
England. The SDSS Web site is http://www.sdss.org/.
(End) Patricia Vannier [CDS] 16-Nov-2022