J/MNRAS/466/2570 Low ionization emission-line regions galaxies (Belfiore+, 2017)
SDSS-IV MaNGA -
the spatially resolved transition from star formation to quiescence.
Belfiore F., Maiolino R., Maraston C., Emsellem E., Bershady M.A.,
Masters K.L., Bizyaev D., Boquien M., Brownstein J.R., Bundy K.,
Diamond-Stanic A.M., Drory N., Heckman T.M., Law D.R., Malanushenko O.,
Oravetz A., Pan K., Roman-Lopes A., Thomas D., Weijmans A.-M.,
Westfall K.B., Yan R.
<Mon. Not. R. Astron. Soc., 466, 2570-2589 (2017)>
=2017MNRAS.466.2570B 2017MNRAS.466.2570B (SIMBAD/NED BibCode)
ADC_Keywords: Galaxies, nearby ; Redshifts ; Morphology ; Photometry, SDSS
Keywords: galaxies: evolution - galaxies: fundamental parameters -
galaxies: ISM
Abstract:
Using spatially resolved spectroscopy from SDSS-IV MaNGA we have
demonstrated that low ionization emission-line regions (LIERs) in
local galaxies result from photoionization by hot evolved stars, not
active galactic nuclei, hence tracing galactic region hosting old
stellar population where, despite the presence of ionized gas, star
formation is no longer occurring. LIERs are ubiquitous in both
quiescent galaxies and in the central regions of galaxies where star
formation takes place at larger radii. We refer to these two classes
of galaxies as extended LIER (eLIER) and central LIER (cLIER)
galaxies, respectively. cLIERs are late-type galaxies primarily spread
across the green valley, in the transition region between the star
formation main sequence and quiescent galaxies. These galaxies display
regular disc rotation in both stars and gas, although featuring a
higher central stellar velocity dispersion than star-forming galaxies
of the same mass. cLIERs are consistent with being slowly quenched
inside-out; the transformation is associated with massive bulges,
pointing towards the importance of bulge growth via secular evolution.
eLIERs are morphologically early types and are indistinguishable from
passive galaxies devoid of line emission in terms of their stellar
populations, morphology and central stellar velocity dispersion.
Ionized gas in eLIERs shows both disturbed and disc-like kinematics.
When a large-scale flow/rotation is observed in the gas, it is often
misaligned relative to the stellar component. These features indicate
that eLIERs are passive galaxies harbouring a residual cold gas
component, acquired mostly via external accretion. Importantly,
quiescent galaxies devoid of line emission reside in denser
environments and have significantly higher satellite fraction than
eLIERs. Environmental effects thus represent the likely cause for the
existence of line-less galaxies on the red sequence.
Description:
We study the properties of galaxies based on their spatially resolved
ionized gas emission. We make use of spatially resolved spectroscopy
for a sample of 586 galaxies from SDSS-IV MaNGA.
The sample is presented in table B.
Direct any queries to Francesco Belfiore, fb338(at)cam.ac.uk.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tableb.dat 145 586 Identifiers and fundamental properties (table B1)
and Photometric and morphological properties
(table B2) of the galaxy sample used in this work
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See also:
J/MNRAS/435/2835 : Morphological types from Galaxy Zoo 2 (Willett+, 2013)
Byte-by-byte Description of file: tableb.dat
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Bytes Format Units Label Explanations
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1- 9 A9 --- MaNGA MaNGA ID (NN-NNNNN)
11- 16 I6 --- NSA NSA ID (1)
18- 27 F10.6 deg RAdeg NSA right ascension (J2000) (1)
29- 37 F9.6 deg DEdeg NSA declination (J2000) (1)
39- 43 F5.3 --- z NSA redshift (1)
45- 49 I5 --- Plate MaNGA plate
51- 55 I5 --- IFU MaNGA ifudesign
57- 62 F6.3 [Msun] logM* NSA Log of stellar mass, from K-correction,
ωM=0.3, H0=70
64- 69 F6.3 [Msun/yr] logSFR ? MaNGA star formation rate, calculated
following Appendix A
70 A1 --- n_logSFR [i] i for infinity
72- 78 F7.3 arcsec Re NSA, Sersic effective radius
80- 84 A5 --- Class MaNGA Emission line class, from LIER Paper I
(Belfiore et al., 2016MNRAS.461.3111B 2016MNRAS.461.3111B) (2)
86- 90 F5.3 --- b/a NSA, Sersic b/a axis ratio
92- 96 F5.3 --- n NSA, Sersic n index
98-104 F7.3 deg phi NSA, Sersic position angle
106-110 F5.3 --- R90/R50 NSA, Concentration index, C=R90/R50
112-116 F5.3 --- GZPdisc Galaxy Zoo 2, p_disc, from Willet et al.,
2013, Cat. J/MNRAS/435/2835
118-124 F7.3 km/s sigma* ? MaNGA, stellar velocity dispersion
within 0.5Re
126-131 F6.3 mag NUV-r NSA, NUV-r colour index
133-138 F6.3 mag u-r NSA, u-r colour index
140-145 F6.3 mag g-r NSA, g-r colour index
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Note (1): From NASA-Sloan catalogue (NSA),
(NSA v101, http://www.sdss.org/dr13/manga/manga-target-selection/nsa,
Blanton et al. 2011AJ....142...31B 2011AJ....142...31B).
Note (2): Class code as follows:
SF = star forming
cLIER = central LIER
eLIER = extended LIER
LL = line less
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History:
From electronic version of the journal
References:
Belfiore et al., Paper I 2016MNRAS.461.3111B 2016MNRAS.461.3111B
(End) Patricia Vannier [CDS] 16-Oct-2019