J/ApJ/953/27 Dusty ellipticals (Lesniewska+, 2023)
The fate of the interstellar medium in early-type galaxies.
II. Observational evidence for morphological quenching.
Lesniewska A., Michalowski M.J., Gall C., Hjorth J., Nadolny J., Ryzhov O.,
Solar M.
<Astrophys. J., 953 27 (2023)>
=2023ApJ...953...27L 2023ApJ...953...27L (SIMBAD/NED BibCode)
ADC_Keywords: Galaxies, IR ; Interstellar medium ; Morphology
Keywords: early-type galaxies - elliptical galaxies - galaxy ages -
galaxy evolution - galaxy quenching - interstellar medium -
dust destruction
Abstract:
The mechanism by which galaxies stop forming stars and get rid of
their interstellar medium (ISM) remains elusive. Here, we study a
sample of more than 2000 elliptical galaxies in which dust emission
has been detected. This is the largest sample of such galaxies ever
analyzed. We infer the timescale for removal of dust in these galaxies
and investigate its dependence on physical and environmental
properties. We obtain a dust-removal timescale in elliptical galaxies
of tau=2.26±0.18Gyr, corresponding to a half-life time of
1.57±0.12Gyr. This timescale does not depend on environment, stellar
mass, or redshift. We observe a departure of dusty elliptical galaxies
from the relation between star formation rate and dust mass. This is
caused by the star formation rates declining faster than the dust
masses and indicates that there exists an internal mechanism that
affects star formation but leaves the ISM intact. Morphological
quenching together with ionization or outflows caused by older stellar
populations (Type Ia supernovae or planetary nebulae) is consistent
with these observations.
Description:
Based on the analysis of dusty early-type galaxies (ETGs) selected
from the GAMA database. Dusty ETGs were selected based on: the
redshift range 0.01<z<0.32, Sersic index >4, and Hershel S250
flux S/N>3.
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
dusty.dat 442 2050 Main catalogue containing all parameters
examined in the paper
--------------------------------------------------------------------------------
See also:
J/MNRAS/413/971 : Galaxy And Mass Assembly (GAMA) DR1 (Driver+, 2011)
J/MNRAS/452/2087 : Galaxy And Mass Assembly (GAMA) DR2 (Liske+, 2015)
J/MNRAS/474/3875 : Galaxy And Mass Assembly (GAMA) DR3 (Baldry+, 2018)
Byte-by-byte Description of file: dusty.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 7 I7 --- CATAID Unique ID of GAMA object (CATAID_1)
9- 14 F6.4 --- z Spectroscopic redshift (Z_1)
16- 21 F6.3 Msun M*2.5 2.5th percentile of total mass of stars ever
formed (massstellarpercentile2_5)
23- 28 F6.3 Msun M*16 16th percentile of total mass of stars ever
formed (massstellarpercentile16)
30- 35 F6.3 Msun M*50 50th percentile of total mass of stars ever
formed (massstellarpercentile50)
37- 42 F6.3 Msun M*84 84th percentile of total mass of stars ever
formed (massstellarpercentile84)
44- 49 F6.3 Msun M*97.5 97.5th percentile of total mass of stars
ever formed (massstellarpercentile97_5)
51- 55 F5.3 Msun Mdust2.5 2.5th percentile of total mass of dust
(massdustpercentile2_5)
57- 61 F5.3 Msun Mdust16 16th percentile of total mass of dust
(massdustpercentile16)
63- 67 F5.3 Msun Mdust50 50th percentile of total mass of dust
(massdustpercentile50)
69- 73 F5.3 Msun Mdust84 84th percentile of total mass of dust
(massdustpercentile84)
75- 79 F5.3 Msun Mdust97.5 97.5th percentile of total mass of dust
(massdustpercentile97_5)
81- 86 F6.3 Msun/yr SFR2.5 2.5th percentile of star formation rate
(SFR01Gyrpercentile25)
88- 93 F6.3 Msun/yr SFR16 16th percentile of star formation rate
(SFR01Gyr_percentile16)
95-100 F6.3 Msun/yr SFR50 50th percentile of star formation rate
(SFR01Gyr_percentile50)
102-107 F6.3 Msun/yr SFR84 84th percentile of star formation rate
(SFR01Gyr_percentile84)
109-114 F6.3 Msun/yr SFR97.5 97.5th percentile of star formation rate
(SFR01Gyrpercentile975)
116-120 F5.3 yr Ager2.5 2.5th percentile of r-band light-weighted age
(agerpercentile25)
122-126 F5.3 yr Ager16 16th percentile of r-band light-weighted age
(ager_percentile16)
128-132 F5.3 yr Ager50 50th percentile of r-band light-weighted age
(ager_percentile50)
134-138 F5.3 yr Ager84 84th percentile of r-band light-weighted age
(ager_percentile84)
140-144 F5.3 yr Ager97.5 97.5th percentile of r-band light-weighted
age (agerpercentile975)
146-157 F12.8 deg RAdeg Right Ascension (J2000) (RA_1)
159-169 E11.8 deg DEdeg Declination (J2000) (DEC_1)
171-186 F16.9 arcsec GALre-r GALFIT effective radius (GALRE_r)
188-194 F7.4 --- GALn-r GALFIT Sersic index (GALINDEX_r)
196-205 E10.8 arcsec e_GALre-r ?=-9999 GALFIT error on Sersic index
(GALREERR_r)
207-215 E9.4 --- e_GALn-r ?=-9999 GALFIT error on effective radius
(GALINDEXERR_r)
217-228 E12.10 Jy F100 ?=-999 Herschel PACS 100 micron flux
(P100_flux)
230-244 F15.10 Jy e_F100 ?=-999 Error in Herschel PACS 100 micron flux
(P100_fluxerr)
246-257 E12.10 Jy F160 ?=-999 Herschel PACS 160 micron flux
(P160_flux)
259-273 F15.10 Jy e_F160 ?=-999 Error in Herschel PACS 160 micron flux
(P160_fluxerr)
275-286 F12.10 Jy F250 Herschel SPIRE 250 micron (S250_flux)
288-299 F12.10 Jy e_F250 Error in Herschel SPIRE 250 micron
(S250_fluxerr)
301-313 E13.10 Jy F350 Herschel SPIRE 350 micron (S350_flux)
315-326 F12.10 Jy e_F350 Error in Herschel SPIRE 350 micron
(S350_fluxerr)
328-340 E13.10 Jy F500 ?=-999 Herschel SPIRE 500 micron (S500_flux)
342-356 F15.10 Jy e_F500 ?=-999 Error in Herschel SPIRE 500 micron
(S500_fluxerr)
358-373 F16.9 --- D4000N ? 4000Å break strength (D4000N)
375-391 F17.10 --- e_D4000N ? Uncertainty on the 4000Å break strength
(D4000N_ERR)
393-398 F6.3 Mpc DistTo5nn ? Distance to 5th nearest neighbour in
co-moving units (DistanceTo5nn)
400-406 F7.3 Mpc-2 SurDens ? Surface density based on the distance to
the 5th nearest neighbour (SurfaceDensity)
408-414 E7.4 Mpc-2 e_SurDens ? Surface density uncertainty
(SurfaceDensityErr)
416 I1 --- f_SurDens [0/2]? Flag indicating problems with surface
density measurement (SurfaceDensityFlag)
418-438 E21.19 --- Mdust/M* Dust-to-Stellar mass ratio (dust/stellar)
440-442 A3 --- Type [MSb ] Main sequence galaxies (MS) and
below-MS galaxies (bMS) (type)
--------------------------------------------------------------------------------
History:
From Aleksndra Lesniewska, aleksandra.lesniewska(at)amu.edu.pl
Acknowledgements:
This work was supported by the support of the National Science Centre,
Poland through the SONATA BIS grant 2018/30/E/ST9/00208.
This research was funded in whole or in part by National Science
Centre, Poland (grant number: 2021/41/N/ST9/02662).
This work was supported by the support of the Leon Rosenfeld
Foundation, of Adam Mickiewicz University in Poznan, Poland via
program Uniwersytet Jutra II (POWR.03.05.00-00-Z303/18), of the
National Science Centre, Poland through the grant 2022/01/4/ST9/00037.
This work is supported by a VILLUM FONDEN Investigator grant (project
number 16599) and a Young Investigator Grant (project number 25501).
References:
Michalowski et al., Paper I 2019A&A...632A..43M 2019A&A...632A..43M
Michalowski et al., Paper III 2024ApJ...964..129M 2024ApJ...964..129M
(End) Patricia Vannier [CDS] 17-Jun-2024