Galaxy Evolution interstellar matter (ISM) drives galaxy evolution, - - PowerPoint PPT Presentation

SFR evolution driven by gas supply ?? starburst vs main sequence ?? Galaxy Evolution interstellar matter (ISM) drives galaxy evolution, but … need to measure the mass of ISM gas or dust CO / long λ dust em. w/ ALMA è high J CO ?? physical understanding of RJ

dust in rad. equil. -- heated by photons from : stars + AGN

• ther dust, ie. secondary photons

dust in rad. equil. -- heated by photons from : stars + AGN

• ther dust, ie. secondary photons

dust cloud spectrum -- w/ increasing Mdust

• peak shifts to longer λ for increased τ (or dust mass)
• flux on long λ tail scales linearly with Mdust

Scoville, 2011 Canary Is. winter school lectures

L = 1012 L¤ Mdust= 108 è 6x109M¤

empirically calibrate w/ low z normal galaxies and ULIRGs + high z SMGs

Lν ∝ T

Dκν

dust gas Mgas

RJ dust continuum optically thin,

What TD ? è adopt simple constant 25 K regions of higher T relatively small frac. of mass Orion GMCs Lombardi etal 2014 Auriga-California GMC Harvey etal 2013

• nly 2% of mass in high T (25 K) region of LkHα 101

most at ~15 K

204 206 208 210 212 214 216 Galactic Longitude 22 20 18 16 14 12 Galactic Latitude

O r i o n A O r i o n B M o n R 2

NGC 2024 NGC 2068 NGC 2071 NGC 1977 OrionNebula 10 pc

• Fig. 2. Composite three-color image showing the Herschel/SPIRE intensities for the region considered, where available (with the 250 µm, 350 µm,

and 500 µm bands shown in blue, green, and red). For regions outside the Herschel coverage, we used the Planck/IRAS dust model (τ , T, β) to

204 206 208 210 212 214 216 Galactic Longitude 22 20 18 16 14 12 Galactic Latitude 204 206 208 210 212 214 216 Galactic Longitude 22 20 18 16 14 12 Galactic Latitude

O r i o n A O r i o n B M o n R 2

NGC 2024 NGC 2068 NGC 2071 NGC 1977 OrionNebula 10 pc

Auriga – California GMC (Harvey etal 2013) 70 μm hot dust extended over ~10 arcmin, cold dust 6 deg

dust mass TD Auriga – California GMC 70 μm 2% of mass in hot region !!

6.7x1019 erg/s/Hz/M¤ w/ less than factor 2 dispersion Planck: Milky Way è 6.2x1019 erg/s/Hz/M¤ β = 1.8 +- 0.1 empirical basis for RJ continuum è ISM masses quick and reliable !! factor 2

Hughes etal ‘17 get 6.4x1019 for 67 MS gal. @ z < 0.3

RJ dust continuum è ISM masses ALMA w/ ~2 min integrations (CO 100x longer) 1011 pointings w/i COSMOS field è 687 detections of Herschel far infrared sources !!

w/ Vanden Bout, Lee, Sheth, Aussel, Capak , Sanders, Bongiorno, Diaz-Santos, Casey, Murchikova, Koda, Laigle, Darvish, Vlahakis, McCracken, Ilbert, Pope, Chu, Toft, Ivison, Morokuma-Matsui, Armus, Masters

ISM evolution z = 0.3 to 3

• Dunne etal mid z samples è dust mass
• Fujimoto – sizes of dust em.

logic of this work : all ALMA 1.3 mm & 850 μm obs. in COSMOS field search for sources at positions of Herschel FIR sources (14000) all Herschel sources w/i FOVs detected !! è 687 detections functional dependence of :

• 1. ISM ( z, M*, sSFR rel. to MS)
• 2. SFR / ISM ( z, sSFR rel. to MS, M* )
• 3. Accretion rates needed to maintain SF

MISM Mstellar z

SFR MISM

gas contents correlated w/ ??

• time in cosmic history ( z )
• mass of galaxy ( Mstellar )
• starburst vs main sequence ( sSFR / sSFRMS )

gas contents correlated with :

• time in cosmic history ( z )
• mass of galaxy ( Mstellar )
• starburst vs main sequence ( sSFR / sSFRMS )

MISM = 7.07×10

9Msun 1+z

( )

1.84

sSFR sSFRMS ⎛ ⎝ ⎜ ⎞ ⎠ ⎟

0.32

Mstellar 10

10Msun

⎛ ⎝ ⎜ ⎞ ⎠ ⎟

0.30

SF law : MISM SFR z efficiencies z sSFR/sSFRMS MISM SFR SFR Msunyr

−1

( ) /

MISM 10

9Msun

⎛ ⎝ ⎜ ⎞ ⎠ ⎟ = 0.31 1+ z

( )

1.05

sSFR sSFRMS ⎛ ⎝ ⎜ ⎞ ⎠ ⎟

0.70

Mstellar 10

10Msun

⎛ ⎝ ⎜ ⎞ ⎠ ⎟

0.01

covariances from Monte Carlo Markov Chain fitting well-behaved w/ single values uncertainties ~0.1 in exponents

ISM fit covariances SFR fit covariances

MISM = 7.07×10

9MΘ 1+ z

( )

1.84

sSFR sSFRMS ⎛ ⎝ ⎜ ⎞ ⎠ ⎟

0.32

Mstellar 10

10Msun

⎛ ⎝ ⎜ ⎞ ⎠ ⎟

0.30

• evolution w/ z : due to both increase in ISM and SF eff.
• increase above MS for SBs : higher ISM and SF eff.
• ISM varies as Mstellar

0.3 and SF eff. indep. of Mstellar

• not a simple low-z KS law -- higher efficiency H2 è *’s
• efficiencies

SFR Msunyr

−1

( ) /

MISM 10

9Msun

⎛ ⎝ ⎜ ⎞ ⎠ ⎟ = 0.31 1+ z

( )

1.05

sSFR sSFRMS ⎛ ⎝ ⎜ ⎞ ⎠ ⎟

0.70

Mstellar 10

10Msun

⎛ ⎝ ⎜ ⎞ ⎠ ⎟

0.01

evolution rel. to z = 0 z

why ? MS (1+z)2.9 (1+z)1.8 (1+z)1.1

gas depletion times ISM mass fractions at z > 2, ~500 Myr MS 30% -- 80% above MS è accretion MISM/SFR (108 yrs) MISM/(Mstellar+MISM) z z

dMISM dt = − 0.7 SFR + M

• accretion

evolutionary continuity of MS

SFR Mstellar accretion needed to maintain SF :

M

• acc = 1.12 Msunyr−1 • 1+ z

( )3.6

Mstellar 1010Msun ⎛ ⎝ ⎜ ⎜ ⎞ ⎠ ⎟ ⎟ 0.44

accretion rates are huge : 100 Msunyr-1 at z > 2

SFRs - color ISM mass - color

accretion rate (M¤ yr-1) -- contours

z z Mstellar Mstellar z

cosmic evolution SF SFRD mass density z z

Madau & Dickenson ‘13

cosmic evol. of ISM and stellar mass

• verall cosmic evolution

summary :

• 1. RJ dust continuum is fast (2min) and reliable
• 2. ISM content and SFE evolve each less rapidly w/ z than SFR
• 3. ISM mass varies as Mstellar

0.3

• 4. above MS, SB due to both increased ISM and higher eff.
• 5. accretion rate are huge ~ 100 Msun yr-1

specific accretion rate (Macc / Mstellar ) :

==> lower at high Mstellar

Ÿ

Arp 220 -- double nuclei (separation è 412 pc) 11 km baselines !! è 90 mas resolution è 35 pc è resolves nuclear disks !!

• w/ Murchikova, Walter, Koda, Vanden Bout, Vlahakis, Barnes, Armus, Yun,

Sheth, Sanders, Cox, Zschaechner, Tacconi, Torrey, Hayward, Thompson, Genzel, Robertson, Hernquist, Hopkins, van der Werf, Decarli

1 arcsec è 361 pc Arp 220 @ 77 Mpc LIR = 2.5x1012 L¤

• West

East huge dust extinction towards nuclei !! è ALMA 2μm HST image 0.2’’ res.

integrated CO line and <V> (0,0 = continuum peaks)

Arp 220 East CO (1-0)!

total flux ! <V> !

Arp 220 West CO (1-0)!

<V> ! total ! flux !

total emission è velocities è

1 arcsec è 361 pc Arp 220 @ 77 Mpc 2μm LIR = 2.5x1012 L¤

• West

East A ~ 2000 mag tow

Arp 220 East ! continuum 2.6 mm! Arp 220 West ! continuum 2.6 mm!

at 2.6 mm dust emission West TB = 120 K ~ TD è optically thick

2.6 mm dust continuum

70 pc NB : TB ~ 200 K è TD > 200 K , yet TFIR ~ 38 K !!

peak shifts to longer λ for increased τ L = 1012 L¤ Mdust= 108 è 6x109M¤

at 2.6 mm dust emission West TB = 120 K (expect ~170 K for 1012 L¤ R ~ 15 pc)

• è τ ~ 1 at 2.6 mm !!
• è NH2 = 2x1026 cm-2 , AV = 105 mags !!
• MISM (west compact nucleus) ~ 2x109 M¤ R < 16 pc
• nH2 ~ 106 cm-3
• dust column è AV = 105 mags !!!!!!!!

at 2.6 mm dust emission West TB = 120 K (expect ~170 K for 1012 L¤ R ~ 15 pc)

• è τ ~ 1 at 2.6 mm !!
• è NH2 = 2x1026 cm-2 , AV = 105 mags !!
• MISM (west compact nucleus) ~ 2x109 M¤ R < 16 pc
• nH2 ~ 106 cm-3
• dust column è AV = 105 mags !!!!!!!!
• = 200 gr cm-2
• ~ 1 ft thick wall of GOLD !!

summary :

• measure ISM rapidly (2min) w/ RJ dust continuum

gas contents ~ 50% of mass, ‘SB gal.’ have more gas SF law w/ dep. time ~ 500 Myr at high z and above MS more gas and higher eff. (SF/Mgas)

• 90 mas imaging of Arp 220 resolves nuclear disks
• disk masses from dust cont., CO 1-0 & rotation curves

agree w/i factor 2-3

• bscuration wall !!

dust/gas ratio (Draine etal ‘07) solid points with good sub-mm and CO & HI

dust/gas ratio (Draine etal ‘07) solid points with good sub-mm and CO & HI è ~constant ratio for Z¤ to Z¤/3

Mdust / MHI+H2!

0.1! 0.001! 8.2! 8! 8.6! 0.01! 8.4!

12 + log10 (O/H)gas! Mdust / Mgas for galaxies w/ !

SCUBA and CO & HI maps!

(Draine etal 2007)!

my ?? ‒ a puzzle : Arp 220 W ‒ dust peak on nucleus , CO hole

Arp 220 West ! continuum 2.6 mm!

total flux !

Arp 220 West CO (1-0)!

why ? ( 1 £ !!)

• cont. – sub

CO