A FURTHER LOOK INTO QUENCHING: TEARING APART THE MAIN SEQUENCE INTO ITS BULGE, DISK AND GAS CONTENT

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Tobias Anderson
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1 A FURTHER LOOK INTO QUENCHING: TEARING APART THE MAIN SEQUENCE INTO ITS BULGE, DISK AND GAS CONTENT, Corentin Schreiber, David Elbaz, Laure Ciesla and the CANDELS+GOODS+Herschel folks

2 THE MAIN SEQUENCE PROPAGANDA Scatter is ~0.3 dex at all stellar masses and all redshifts up to z~4 Galaxies on the MS produce more than 70% of present day stars The Main Sequence is the dominant mode of star formation at least up to z ~4 (Schreiber, MP et al., 2015) 2

3 THE MAIN SEQUENCE PROPAGANDA Scatter is ~0.3 dex at all stellar masses and all redshifts up to z~4 Galaxies on the MS produce more than 70% of present day stars The Main Sequence is the dominant mode of star formation at least up to z ~4 Starbursts fraction is constant with z Account for ~15% of the CSFR (Schreiber, MP et al., 2015) 3

4 THE MAIN SEQUENCE BENDING A varying slope with redshift/mass (Schreiber, MP et al., 2015) 4

5 THE MAIN SEQUENCE BENDING z=4 z=2.3 z=0.7 z=0.5 (Schreiber, MP et al., 2015) (Whitaker et al., 2014 but see also Karim et al., 2011; Whitaker et al., 2012; Magnelli et al., 2014 and others ) 5

6 THE MAIN SEQUENCE BENDING A varying slope with redshift/mass Is there a growing component that increases the stellar mass but not the SFR? Bulges? (Schreiber, MP et al., 2015) 6

7 SSFR SSFR THE MAIN SEQUENCE BENDING A varying slope with redshift/mass Is there a growing component that increases the stellar mass but not the SFR? Bulges? (Abramson et al., 2014) 7

8 THE MAIN SEQUENCE BENDING A varying slope with redshift/mass Is there a growing component that increases the stellar mass but not the SFR? Bulges? Is the SFR lower because of gas depletion? (Gavazzi et al., 2015) (Schreiber, MP et al., 2015) Or a decreasing efficiency in converting gas to stars? 8

9 Sample: CANDELS fields 0.7 < z < 1.3 H < 22.5 (Log M > 10.2) Spitzer/Herschel detections (SFR = SFR IR + SFR UV ) (Schreiber et al., 2016) 9

10 GIM2D bulge+disk model (Schreiber et al., 2016) 10

11 B/T = (M - M disk )/M B/T = 0 pure disk B/T = 1 pure bulge (Schreiber et al., 2016) Corrected for mass-to-light ratios of bulge and disk Tested with simulations 11

12 B/T < 0.2 B/T > 0.8 GIM2D bulge+disk model Tested with simulations (Schreiber et al., 2016) Corrected for mass-to-light ratios of bulge and disk B/T = (M - M disk )/M B/T < 0.2 pure disk B/T > 0.8 pure bulge 12

13 BULGES, DISKS AND B/T < 0.2 B/T GAS > 0.8 ON THE MAIN SEQUENCE (Schreiber et al., 2016) GIM2D bulge+disk model Tested with simulations Corrected for mass-to-light ratios of bulge and disk B/T = (M - Mdisk)/M B/T < 0.2 pure disk B/T > 0.8 pure bulge 13

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16 bending still present with disks only bulges are not the answer 16

17 A varying slope with redshift/mass Is there a growing component that increases the stellar mass but not the SFR? Bulges? Is the SFR lower because of gas depletion? (Gavazzi et al., 2015) (Schreiber, MP et al., 2015) Or a decreasing efficiency in converting gas to stars? 17

18 (UVJ selected) 18

19 Galliano+11 (UVJ selected) 19

20 (UVJ selected) Galliano+11 M dust M gas = (1/Z) x (1-f)/f x M dust Franco & Cox 86 Z: metallicity f: % of metals in dust FMR, Manucci+10 Leroy+08, Magdis+12 Assuming: single dust grain composition M* - SFR - Z relation fixed value of f 20

21 Assuming: M gas = (1/Z) x (1-f)/f x M dust single dust grain composition Franco & Cox 86 M* - SFR - Z relation Z: metallicity f: % of metals in dust fixed value of f FMR, Manucci+10 Leroy+08, Magdis+12 Cross-checked with HI+CO at z=0 21

22 M gas = (1/Z) x (1-f)/f x M dust Franco & Cox 86 Z: metallicity f: % of metals in dust FMR, Manucci+10 Leroy+08, Magdis+12 Assuming: single dust grain composition M* - SFR - Z relation fixed value of f Cross-checked with HI+CO at z=0 22

23 slow downfall of SFE in massive galaxies! z=2 z=2 z=1 z=1 z=0 z=0 23

24 TAKE ME HOME the Main Sequence has a varying slope flattens at high stellar mass and low redshift not linked to bulge growth or gas deficit due to a downfall of star formation efficiency 24

arxiv: v3 [astro-ph.ga] 21 Jan 2016

arxiv: v3 [astro-ph.ga] 21 Jan 2016 Astronomy & Astrophysics manuscript no. paper c ESO 2018 October 17, 2018 Observational evidence of a slow downfall of star formation efficiency in massive galaxies during the last 10 Gyr C. Schreiber