J/ApJ/923/28 Metallicity gradients from GASP & MaNGA surveys (Franchetto+, 2021)
GASP and MaNGA surveys shed light on the enigma of the gas metallicity gradients
in disk galaxies.
Franchetto A., Mingozzi M., Poggianti B.M., Vulcani B., Bacchini C.,
Gullieuszik M., Moretti A., Tomicic N., Fritz J.
<Astrophys. J., 923, 28 (2021)>
=2021ApJ...923...28F 2021ApJ...923...28F
ADC_Keywords: Spectra, optical; Abundances; Galaxies, nearby; Surveys
Keywords: Galaxy disks ; Galaxy clusters ; Field galaxies ; Metallicity ;
Galaxy chemical evolution
Abstract:
Making use of both MUSE observations of 85 galaxies from the survey
GASP (GAs Stripping Phenomena in galaxies with MUSE) and a large
sample from MaNGA (Mapping Nearby Galaxies at Apache Point Observatory
survey), we investigate the distribution of gas metallicity gradients
as a function of stellar mass for local cluster and field galaxies.
Overall, metallicity profiles steepen with increasing stellar mass up
to 1010.3M☉ and flatten out at higher masses. Combining the
results from the metallicity profiles and the stellar mass surface
density gradients, we propose that the observed steepening is a
consequence of local metal enrichment due to in situ star formation
during the inside-out formation of disk galaxies. The metallicity
gradient-stellar mass relation is characterized by a rather large
scatter, especially for 109.8<M*/M☉<1010.5, and we
demonstrate that metallicity gradients anti-correlate with the galaxy
gas fraction. Focusing on the galaxy environment, at any given stellar
mass, cluster galaxies have systematically flatter metallicity
profiles than their field counterparts. Many subpopulations coexist in
clusters: galaxies with shallower metallicity profiles appear to have
fallen into their present host halo sooner and have experienced the
environmental effects for a longer time than cluster galaxies with
steeper metallicity profiles. Recent galaxy infallers, like galaxies
currently undergoing ram pressure stripping, show metallicity
gradients more similar to those of field galaxies, suggesting they
have not felt the effect of the cluster yet.
Description:
In this paper we study the radial distribution of ionized gas
metallicity and stellar mass in the GAs Stripping Phenomena in
galaxies with MUSE (GASP; Poggianti+ 2017ApJ...844...48P 2017ApJ...844...48P) sample,
dividing galaxies according to their environment. GASP is an ESO Large
Program that observed 114 galaxies with a spatial resolution of 1kpc
and a sky coverage of, on average, 8 effective radii.
GASP observations were taken by the spectrograph MUSE at the Very
Large Telescope (VLT), with wavelength coverage between 4800 and
9300Å with a spectral resolution between R=1770 and 3590.
The Mapping Nearby Galaxies at Apache Point Observatory survey (MaNGA)
observations were carried out by the 2.5m Sloan Digital Sky Survey
(SDSS) telescope at the Apache Point Observatory with a spectral range
between 3600 and 10300Å and a resolution of R∼1400 at 4000Å and
R∼2600 at 9000Å. The data used in this work are taken from the
MaNGA DR15 catalog (see Wake+ 2017, J/AJ/154/86).
Throughout this work, we use a Λ cold dark matter cosmology
with ΩM=0.3, ΩΛ=0.7, and H0=70km/s/Mpc, and a
Chabrier (2003PASP..115..763C 2003PASP..115..763C) initial mass function (IMF).
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 80 85 Properties of the GASP galaxies
table2.dat 88 85 Best-fit parameters
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See also:
J/MNRAS/416/727 : Padova-Millennium Galaxy and Group Catalogue (Calvi+, 2011)
J/ApJS/208/10 : κ-distribution in HII regions (Dopita+, 2013)
J/A+A/566/A1 : Flux- & volume-limited groups for SDSS gal. (Tempel+, 2014)
J/ApJ/806/16 : CHemical Abundances of Spirals. I. NGC628 (Berg+, 2015)
J/A+A/581/A41 : OmegaWINGS BV phot. of galaxy clusters (Gullieuszik+, 2015)
J/A+A/595/A62 : CALIFA galaxies O/H and N/O slopes (Perez-Montero+, 2016)
J/A+A/587/A70 : CALIFA face-on spiral gal. oxygen (Sanchez-Menguiano+, 2016)
J/A+A/606/A12 : MUSE-Wide survey: 831 emission line galaxies (Herenz+, 2017)
J/AJ/154/86 : MaNGA catalog, DR15 (Wake+, 2017)
J/ApJ/887/80 : Gas phase oxygen abundances for HII regions (Kreckel+, 2019)
J/A+A/626/A14 : XMMXCSJ2215.9-1738 galaxies reduced datacubes (Maier+, 2019)
J/ApJ/895/106 : GAs Stripping Phenomena in gal. with MUSE (Franchetto+, 2020)
J/ApJ/899/13 : GASP. XXI. Star forming rate in 54 gal. (Gullieuszik+, 2020)
J/A+A/649/A39 : xCOLD GASS and xGASS. Metallicity gradients (Lutz+, 2021)
J/ApJ/907/22 : GASP. XXXII. Diffuse Ionized Gas (DIG) (Tomicic+, 2021)
J/A+A/670/A4 : MUSE Hubble Ultra Deep Field surveys. DR2 (Bacon+, 2023)
http://web.oapd.inaf.it/gasp/index.html : GASP home page
Byte-by-byte Description of file: table1.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 12 A12 --- ID Identifier used in this work
14- 15 I2 h RAh Hour of Right Ascension (J2000)
17- 18 I2 min RAm Minute of Right Ascension (J2000)
20- 24 F5.2 s RAs Second of Right Ascension (J2000)
26- 26 A1 --- DE- Sign of the Declination (J2000)
27- 28 I2 deg DEd Degree of Declination (J2000)
30- 31 I2 arcmin DEm Arcminute of Declination (J2000)
33- 38 F6.3 arcsec DEs Arcsecond of Declination (J2000)
40- 40 A1 --- env Environment, F=field, C=cluster
42- 46 F5.2 [Msun] logMs [8.8/11.5] log of stellar mass
48- 51 F4.2 [Msun] e_logMs [0.05/0.2] Lower uncertainty in logMs
53- 56 F4.2 [Msun] E_logMs [0.04/0.1] Upper uncertainty in logMs
58- 63 F6.3 --- aOH [-0.52/0.01] Gas metallicity gradient, dex/Re
65- 69 F5.3 --- e_aOH [0.004/0.1] Uncertainty in aO/H
71- 75 F5.2 --- aMs [-0.95/-0.1] Stellar mass surface density
gradient, dex/Re
77- 80 F4.2 --- e_aMs [0.04/0.2] Uncertainty in aMs
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Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 12 A12 --- ID Identifier used in this work
14- 15 A2 --- func Best-fit function (1)
17- 22 F6.3 --- aOH [-0.52/0.01] Gas metallicity gradient, dex/Re
24- 28 F5.3 --- e_aOH [0.004/0.1] Uncertainty in aOH
30- 34 F5.3 [-] ZRe [8/9.3] Gas metallicity at the effective radius
36- 40 F5.3 [-] e_ZRe [0.006/0.1] Uncertainty in ZRe
42- 45 F4.2 --- Rb [0.5/2.4]? Break radius if func=dl, Re
47- 50 F4.2 --- e_Rb [0.09/0.8]? Uncertainty in Rb
52- 54 F3.1 --- Rin [0.5/1.1]? Inner break radius if func=tl, Re
56- 58 F3.1 --- e_Rin [0.1/0.4]? Uncertainty in Rin
60- 62 F3.1 --- Rout [1.8/2.7]? Outer break radius if func=tl, Re
64- 66 F3.1 --- e_Rout [0.2/0.6]? Uncertainty in Rout
68- 72 F5.2 --- aOHin [-0.4/0.11]? Inner gas metallicity gradient,
dex/Re
74- 77 F4.2 --- e_aOHin [0.02/0.2]? Uncertainty in aOHin
79- 83 F5.2 --- aOHout [-0.15/0.1]? Outer gas metallicity gradient,
dex/Re
85- 88 F4.2 --- e_aOHout [0.03/0.2]? Uncertainty in aOHout
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Note (1): Best-fit function as follows:
sl = single-linear profile;
dl = double-linear profile;
tl = triple-linear profile.
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History:
From electronic version of the journal
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 12-May-2023