J/ApJ/879/131 UV-FIR obs. of post-starburst galaxies & dust masses (Li+, 2019)
The evolution of the interstellar medium in post-starburst galaxies.
Li Z., French K.D., Zabludoff A.I., Ho L.C.
<Astrophys. J., 879, 131 (2019)>
=2019ApJ...879..131L 2019ApJ...879..131L
ADC_Keywords: Galaxies, IR; Interstellar medium; Photometry, ultraviolet;
Photometry, ugriz
Keywords: galaxies: evolution ; galaxies: ISM ; galaxies: starburst ;
infrared: galaxies
Abstract:
We derive dust masses (Mdust) from the spectral energy distributions
of 58 post-starburst galaxies (PSBs). There is an anticorrelation
between specific dust mass (Mdust/M*) and the time elapsed since
the starburst ended, indicating that dust was either destroyed,
expelled, or rendered undetectable over the ∼1Gyr after the burst. The
Mdust/M* depletion timescale, 205-37+58Myr, is consistent with
that of the CO-traced MH2/M*, suggesting that dust and gas are
altered via the same process. Extrapolating these trends leads to the
Mdust/M* and MH2/M* values of early-type galaxies (ETGs)
within 1-2Gyr, a timescale consistent with the evolution of other PSB
properties into ETGs. Comparing Mdust and MH2 for PSBs yields a
calibration, log MH2=0.45logMdust+6.02, that allows us to place
33 PSBs on the Kennicutt-Schmidt (KS) plane, ΣSFR-ΣMH2.
Over the first ∼200-300Myr, the PSBs evolve down and off of the KS
relation, as their star formation rate (SFR) decreases more rapidly
than MH2. Afterwards, MH2 continues to decline whereas the SFR
levels off. These trends suggest that the star formation efficiency
bottoms out at 10-11/yr and will rise to ETG levels within
0.5-1.1Gyr afterwards. The SFR decline after the burst is likely due
to the absence of gas denser than the CO-traced H2. The mechanism of
the Mdust/M* and MH2/M* decline, whose timescale suggests
active galactic nucleus/low-ionization nuclear emission-line region
feedback, may also be preventing the large CO-traced molecular gas
reservoirs from collapsing and forming denser star-forming clouds.
Description:
In this work, we combine three well-studied post-starburst galaxy
(PSB) samples from French+ (2018, J/ApJ/862/2),
Alatalo+ (2016, J/ApJS/224/38), and Rowlands+ (2015MNRAS.448..258R 2015MNRAS.448..258R) to
make the time baseline since the starburst ends as wide as possible.
Our combined PSB sample ranges in post-burst age from ~-100 to ∼800Myr.
We establish UV to FIR SEDs for our PSB sample. We incorporate the
processed WISE and Herschel data from Smercina+ (2018ApJ...855...51S 2018ApJ...855...51S)
for 33 PSBs from French+ (2015ApJ...801....1F 2015ApJ...801....1F) and compile other data
from different catalogs. In addition to compiling the Herschel data
from PACS/SPIRE Point Source Catalogs, we utilize the archival
photometric data from GALEX, SDSS, 2MASS, and WISE (see Section 3).
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 204 58 Archival UV to NIR photometry
table2.dat 152 58 Archival MIR-FIR photometry
table4.dat 84 58 Galaxy properties
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See also:
VII/233 : The 2MASS Extended sources (IPAC/UMass, 2003-2006)
VI/139 : Herschel Observation Log (Herschel Science Centre, 2013)
II/328 : AllWISE Data Release (Cutri+ 2013)
V/147 : The SDSS Photometric Catalogue, Release 12 (Alam+, 2015)
II/335 : Revised cat. of GALEX UV sources (GUVcat_AIS GR6+7) (Bianchi+ 2017)
J/ApJ/703/517 : The Spitzer Local Volume Legacy: IR photometry (Dale+, 2009)
J/A+A/543/A161 : Submm obs. of 323 HRS nearby galaxies (Ciesla+, 2012)
J/ApJ/745/95 : Herschel FIR & submm phot. of KINGFISH sample (Dale+, 2012)
J/MNRAS/420/1684 : End of red sequence galaxies in Galaxy Zoo (Wong+, 2012)
J/A+A/562/A21 : AGN feedback from CO observations (Cicone+, 2014)
J/MNRAS/441/1017 : Multiwavelength photometry of 34 galaxies (Rowlands+, 2014)
J/ApJS/224/38 : SPOGS. I. SDSS Shocked POststarburst Gal. (Alatalo+, 2016)
J/ApJ/862/2 : Post-starburst galaxy ages from SDSS (French+, 2018)
Byte-by-byte Description of file: table1.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 5 A5 --- ID Source identifier (G1)
7- 15 F9.5 deg RAdeg [11.24/343.8] Right Ascension (J2000)
17- 24 F8.5 deg DEdeg [-8.9/64.3] Declination (J2000)
26- 33 E8.2 mJy FFUV [0.0005/0.63]? GALEX FUV band flux density (G2)
35- 42 E8.2 mJy e_FFUV [0.0004/0.05]? Uncertainty in FFUV (G3)
44- 51 E8.2 mJy FNUV [0.003/1] GALEX NUV band flux density (G2)
53- 60 E8.2 mJy e_FNUV [0.0005/0.04] Uncertainty in FNFUV (G3)
62- 69 E8.2 mJy Fu [0.02/2] SDSS DR14 u band flux density (G2)
71- 78 E8.2 mJy e_Fu [0.0018/0.11] Uncertainty in Fu (G3)
80- 87 E8.2 mJy Fg [0.12/8.6] SDSS DR14 g band flux density (G2)
89- 96 E8.2 mJy e_Fg [0.0015/0.3] Uncertainty in Fg (G3)
98-105 E8.2 mJy Fr [0.3/16.2] SDSS DR14 r band flux density (G2)
107-114 E8.2 mJy e_Fr [0.002/0.5] Uncertainty in Fr (G3)
116-123 E8.2 mJy Fi [0.4/22.5] SDSS DR14 i band flux density (G2)
125-132 E8.2 mJy e_Fi [0.003/0.6] Uncertainty in Fi (G3)
134-141 E8.2 mJy Fz [0.58/27.6] SDSS DR14 z band flux density (G2)
143-150 E8.2 mJy e_Fz [0.007/0.9] Uncertainty in Fz (G3)
152-159 E8.2 mJy FJ [0.38/38] 2MASS J band flux density (G2)
161-168 E8.2 mJy e_FJ [0.06/2] Uncertainty in FJ (G3)
170-177 E8.2 mJy FH [0.4/48.6] 2MASS H band flux density (G2)
179-186 E8.2 mJy e_FH [0.06/2.6] Uncertainty in FH (G3)
188-195 E8.2 mJy FKs [0.5/38.6] 2MASS Ks band flux density (G2)
197-204 E8.2 mJy e_FKs [0.1/2.2] Uncertainty in FKs (G3)
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Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 5 A5 --- ID Source identifier (G1)
7- 11 F5.2 mJy F3.4 [0.4/17] AllWISE W1 (3.4um) band flux density (G2)
13- 16 F4.2 mJy e_F3.4 [0.01/1.1] Uncertainty in F3.6 (G3)
18- 22 F5.2 mJy F4.6 [0.3/10.3] AllWISE W2 (4.6um) band flux
density (G2)
24- 27 F4.2 mJy e_F4.6 [0.01/0.7] Uncertainty in F4.6 (G3)
29- 33 F5.2 mJy F12 [0.8/53.5] AllWISE W3 (12um) band flux density (G2)
35- 38 F4.2 mJy e_F12 [0.04/2.6] Uncertainty in F12 (G3)
40 A1 --- l_F22 Limit flag on F22
42- 47 F6.2 mJy F22 [1.7/578]? AllWISE W4 (22um) band flux density (G2)
49- 53 F5.2 mJy e_F22 [0.4/35]? Uncertainty in F22 (G3)
55- 62 F8.2 mJy F70 [7/19700]? Herschel/PACS 70 micron band
flux density (G2)
64- 70 F7.2 mJy e_F70 [2/1410]? Uncertainty in F70 (G3)
72- 79 F8.2 mJy F100 [14/18100]? Herschel/PACS 100 micron band
flux density (G2)
81- 87 F7.2 mJy e_F100 [2/1310]? Uncertainty in F100 (G3)
89- 96 F8.2 mJy F160 [6/10500]? Herschel/PACS 160 micron band
flux density (G2)
98-103 F6.2 mJy e_F160 [2/755]? Uncertainty in F160 (G3)
105-111 F7.2 mJy F250 [10/4150]? Herschel/SPIRE 250 micron band
flux density (G2)
113-118 F6.2 mJy e_F250 [4/294]? Uncertainty in F250 (G3)
120 A1 --- l_F250 Limit flag on F250
122-128 F7.2 mJy F350 [10/1690]? Herschel/SPIRE 350 micron band
flux density (G2)
130-135 F6.2 mJy e_F350 [4/121]? Uncertainty in F350 (G3)
137 A1 --- l_F500 Limit flag on F500
139-144 F6.2 mJy F500 [10/590]? Herschel/SPIRE 500 micron band
flux density (G2)
146-150 F5.2 mJy e_F500 [5/48]? Uncertainty in F500 (G3)
152 A1 --- f_ID [a] a: WISE and Herschel photometry from
Smercina et al. 2018ApJ...855...51S 2018ApJ...855...51S ;
data added by CDS for completeness (1)
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Note (1): WISE and Herschel photometry from Smercina+ 2018ApJ...855...51S 2018ApJ...855...51S
(Tables 7 and 6 taken from the erratum published in 2018, ApJ, 859, 77;
respectively).
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Byte-by-byte Description of file: table4.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 5 A5 --- ID Source identifier (G1)
7- 10 F4.2 arcsec r50 [0.96/7.41] Petrosian radius (2)
12- 16 F5.2 [Msun] logM* [9.6/11.4] log stellar mass (3)
18- 21 F4.2 [Msun] E_logM* [0.06/0.4] Upper uncertainty in logM
23- 26 F4.2 [Msun] e_logM* [0.05/0.6] Lower uncertainty in logM*
28- 31 F4.2 [Msun] logMd [5.3/9] log CIGALE-derived dust mass
33- 36 F4.2 [Msun] e_logMd [0.02/1.1] Uncertainty in logMd
38- 42 F5.2 [-] Ratio [-5/-1.8] log ratio of dust to stellar masses
44- 47 F4.2 [-] e_Ratio [0.1/1.1] Uncertainty in Ratio
49 A1 --- l_logMg Limit flag on logMg
50- 54 F5.2 [Msun] logMg [7.7/10.1] log molecular gas mass (4)
56- 59 F4.2 [Msun] e_logMg [0.02/0.15]? Uncertainty in logMg
61- 65 F5.2 [Msun/yr] SFRun [0.01/28] Uncorrected star formation rate (5)
67- 70 F4.2 [Msun/yr] e_SFRun [0.01/0.9] Uncertainty in SFRun
72 A1 --- l_SFRc Limit flag on SFRc
73- 79 F7.4 [Msun/yr] SFRc [0.0004/12.1]? Star formation
rate corrected for AGN contribution
81- 84 F4.2 [Msun/yr] e_SFRc [0.01/1.3]? Uncertainty in SFRc
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Note (2): From SDSS 14th Data Release (Abolfathi+ 2018ApJS..235...42A 2018ApJS..235...42A).
Containing 50% light.
Note (3): From the SDSS MPA-JHU (Brinchmann+ 2004MNRAS.351.1151B 2004MNRAS.351.1151B and
Tremonti+ 2004ApJ...613..898T 2004ApJ...613..898T) catalog.
Note (4): From French+ (2015ApJ...801....1F 2015ApJ...801....1F), Alatalo+ (2016ApJ...827..106A 2016ApJ...827..106A),
or converted from dust masses if no CO measurement is available
(with an estimated uncertainty of 0.15dex).
Note (5): Derived from Hα fluxes from the MPA-JHU catalog
(corrected for internal dust extinction).
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Global notes:
Note (G1): R1-R11 are from Rowlands+ (2015MNRAS.448..258R 2015MNRAS.448..258R);
EAH01-EAH18, EAS01-EAS15 and F34-F37 are from French+ (2018, J/ApJ/862/2),
and A1-A12 are from Alatalo+ (2016, J/ApJS/224/38).
The data of EAS/EAH sources are presented in Smercina+ (2018ApJ...855...51S 2018ApJ...855...51S).
Note (G2): No correction for extinction has been applied.
Note (G3): The total flux uncertainties correspond to 68% confidence levels.
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History:
From electronic version of the journal
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 15-Dec-2020