The Global Star Formation Laws in Galaxies: Recent Updates

The Global Star Formation Laws in Galaxies: Recent Updates

Yu GaoPurple Mountain ObservatoryChinese Academy of Sciences

May 15, 2012 @5th sino-french

Outline of this talk

• What are the star formation (SF) recipes? SFR-gas (HI, CO) scaling laws: Kennicutt - Schmidt law, SF laws in other forms

• Why do we need a SFR-dense gas law• A linear FIR(SFR)--HCN (dense gas

tracer) relation for all star-forming systems (GMCs-->high-z): SF law in dense gas

• Major issues and debates (CS surveys)• Conclusions

Star formation laws

• Schmidt (1959): SFR~density(HI)^n, n=1-3, mostly 2-3 in ISM of our Galaxy.• Kennicutt (1989): Disk-average [SFR~ density(HI+H2)^n] n is not well constrained. ~1-3, wide spread.• Kennicutt (1998): n=1.4 ? Total gas (HI + H2) vs. Dense gas• Better SF law in dense gas? (Hubble law and H0 analogy)

Hubble law

Kennicutt1998

n=1.4

Normal disk spirals

IR circumnuclear starbursts

SFR vs. M(H2): No Unique Slope:1, 1.4, 1.7?

HI-dominatedLSB galaxies

HI ~ H2

H2-dom

inatedLIR

Gs/

ULIR

Gs

Gao & Solomon 2004b ApJExtragalactic SF=CO until 90’s

Big

iel’s

talk

@S

FR50

SF thresholds maysimply reflect the change of the dominant cold gas phase in galaxiesfrom HI ->H2 & from H2->denseH2

Schruba+2011~linear in H2!

GMCs enbed in diffuse atomic gas（ HI） , the gas reservoir for molecular clouds,and the supply for future star formation. PDRs

Stars are forming in giant molecular clouds (GMCs)

High Density Tracers Merging/interactions trigger gas infall to nuclear regions

Nuclei of Galaxies should possess denser gasas GMCs have to survive to tidal forces (must be denser)

Critical density: the radiating molecule (eg, CO) suffers collisions at the rate: n(H2) sigma v = A (Einstein coefficient A ~ nu^3 mu^2)* High-J (>~3) levels of CO (nu ~ J)higher critical density to be excited (>105cm-3)* & High dipole moment molecules HCN, HNC, HCO+, CS (mu ~ 30x > CO), etc..* X factor ? CO-to-H2, HCN-to-DenseH2 conversions

Dense gas is the essential fuel for high mass star formation in galaxies

HCN Surveys in 53 Galaxies: Gao & Solomon 2004a ApJS

Far-IR, HCN, CO Correlations: Gao & Solomon 2004b ApJ

SFR

Dense Molecular Gas

Baan, Henkel, Loenen + 2008

• Baan et al. (2008)• Kohno 2007, et al. (2003)• Imanishi (2006)• Aalto et al. 2007, 2002, 1995• Solomon et al. 1992• Nguyen et al. 1992• Henkel et al. 1990• Henkel, Baan, Mauersberger 1991

HCN,CS,HNC etc. in SF gals.

Best case studies: Arp 220 & NGC 6240 (Greve + 2009)

13 HCN @high-z

Gao, Carilli, Solomon & Vanden Bout 2007 ApJ, 660, L93

Wu, Evans, Gao et al. 2005 ApJL

Fit to GMCs

Fit to Galaxies

Fit to both GMCs & Gals..

Wu+2010

CARMA+45m CO (Koda + 09)

HST

• Total useful on-source integration time >~110 hours.

• HCN spectra with S/N>3

(a channel width dV ~7 km/s).

• Typical rms ~1-2 mK at dV~20 km/s.

HCN contoursare overlaid onthe CO image

• Correlations between 8um-HCN & 24um-HCN. The solid lines: fixed slope of 1.

SFR

HCN

Chen & Gao in prep.

M33GMCs (Rosolowsky, Pineda & Gao 2011)

∑Mdense vs. ∑SFR

Dense H2 show the best correlation with SFR (linear Liu & Gao 2011).

Liu & Gao arXiv:1106.2813

K-S SF Law in high-redshift galaxiesDaddi et al. 2010; Genzel+2010

CO->H2 conversion factor ?? αco (Msun (K km/s pc2)-1: 4.6 for local spirals 3.6 ± 0.8 for BzKs 0.8 for LIRGs/SMGs/QSOs

Two major SF modes:1. a long-lasting mode for disks (local spirals and BzKs) 2. a rapid starburst for LIRGs ULIRGs & SMGs/QSOs

Bi-modal SF laws in high-z gals (Daddi+2010; Genzel+2010) also exist in local gals

Juneau+2009; Narayanan+2008; Krumholz & Thompson 2007; Iono+2008; Mao+2010 SFR – CO & SFR -- HCN indexes

• Dense gas over a range of 10^4-8 /cm^3

Concluding Remarks

• SF: quiescent (few Dense Cores=DCs), normal, active/burst modes (starbursts: active formation of DCs)

• DCs in Dense Molecular Gas Complexes High Mass Stars/Clusters (SF in different environments: SMGs/hi-z QSOs; ULIRGs/Starbursts; Spirals; LSBs; DCs)

• SF thresholds: change of the dominant cold gas phase in galaxies from HI ->H2 & from H2->denseH2

• (FIR-HCN, CS Linear Correlations) SFR ~ M(DenseH2): the total mass of dense molecular gas in galaxies & all star-forming systems (spanning 10 orders of mag.)?

• SFR-DenseGas: Counting DCs(=SF units) in Galaxies?

Gao & Solomon: Dense H2 DCs/StarsClusters

New Star Formation Law

• Dense Molecular Gas High Mass Stars• SFR ~ M(DENSE) ~ density of dense gas (e.g. gas density >~10^5 cc), linear• HI H2 DENSE H2 Stars

Schmidt law : HI StarsKennicutt : HI + H2 Stars

Gao & Solomon: Dense H2 Stars

From Cores to High-z: Dense GasMassive SF