Topics on HI in the Context of Galaxy Evolution: Baryonic Tully Fisher Relation and its Extension

Topics on HI in the Context of Galaxy Evolution:Baryonic Tully Fisher Relation and its Extension Tsutomu T. TAKEUCHI withHiroshi Jacky ISHIKAWA Division of Particle and Astrophysical Science, Nagoya University, Japan SKA High-z Group Workshop 2013, 20-21 Feb., 2013, Kyoto, Japan

Dark halo • 1. Introduction Darkhalos form and merge with time. Then, first stars and galaxies form and evolve in their potential.

1. Introduction Darkhalos form and merge with time. Then, first stars and galaxies form and evolve in their potential. First stars

Galaxy • 1. Introduction Darkhalos form and merge with time. Then, first stars and galaxies form and evolve in their potential.

1. Introduction Darkhalos form and merge with time. Then, first stars and galaxies form and evolve in their potential.

1. Introduction Darkhalos form and merge with time. Then, first stars and galaxies form and evolve in their potential. The relation between dark halos and galaxies (baryons) is the key to understand the galaxy evolution.

Velocity-luminosity relation The relation between the rotational velocity or velocity dispersion and luminosity of galaxies are tightly correlated. The former is the Tully-Fisher relation, and the latter is the Faber-Jackson relation. In general, we can summarize these relation as the velocity-luminosity relation. Absolute magnitude Willick (1999) Rotational velocity

Velocity-luminosity relation From the virial theorem, we have an approximate relation as follows.

The baryonic Tully-Fisher relation After the first proposal by Tully & Fisher (1977), it was found that at the small circular velocity regime, galaxies tend to deviate downward from the TF relation defined by large galaxies. • More fundamentally, the classical Tully-Fisher relation depends on the observed wavelength because it uses optical/NIR luminosity, which is strongly dependent on the star-formation history.

The baryonic Tully-Fisher relation After the first proposal by Tully & Fisher (1977), it was found that at the small circular velocity regime, galaxies tend to deviate downward from the TF relation defined by large galaxies. • More fundamentally, the classical Tully-Fisher relation depends on the observed wavelength because it uses optical/NIR luminosity, which is strongly dependent on the star-formation history. McGaugh et al. (2000) discovered that if we add the gas mass of galaxies to the stellar mass, we can recover the single power law.

The baryonic Tully-Fisher relation Stellar mass [M☉] Total baryon mass [M☉] McGaugh et al. (2000) Circular velocity[kms-1] • Now, the TF relation appear as a fundamental relation between the baryon mass (galaxy mass) and dynamical mass of a halo.

Relation between dark and baryonic mass functions Example: The functional forms of the halo mass function and galaxy stellar mass function are significantly different. Related to the physics of galaxy formation Somerville & Primack (1999)

Relation between dark and baryonic mass functions Example: The functional forms of the halo mass function and galaxy stellar mass function are significantly different. • There are roughly two different ways to connect the halo mass function and stellar (baryon) mass function. • Velocity-baryonic mass relation • Halo occupation distribution (HOD) Somerville & Primack (1999)

Star-formation main sequence Among empirical relations of galaxies, relations with star formation are also interesting subject. Define the specific star formation rate (SSFR) On the stellar mass-specific SFR plane, there appears a prominent sequence of star-forming galaxies: star-formation main sequence. cf. the blue cloud on the color-magnitude diagram. Schiminovich et al. (2007)

Empirical relations including star formation If we consider the size of galaxies, we may also be interested in the column (surface) density of gas and star formation, leading to the Schmidt-Kennicutt law. The original Schmidt-Kennicutt law is a power-law relation between the surface gas mass density and surface density of the SFR. The slope of this power law is still under debate. Kennicutt & Evans (2012)

Neutral and molecular gas surface density and SFR The SFR is supposed to correlate with dense molecular gas density. However, in the case of the Milky Way, this is not necessarily true. Kennicutt & Evans (2012)

Neutral and molecular gas surface density and SFR The SFR is supposed to correlate with dense molecular gas density. However, in the case of the Milky Way, this is not necessarily true. A comprehensive analysis of the SFR, stellar mass, dynamical mass, and size of galaxies will be ideal. Kennicutt & Evans (2012)

Aim of the study We try to extend the scaling relation of galaxies to incorporate the star formation properties of galaxies. By this analysis, we can connect the halo mass, baryon mass, and their star formation properties. The resulting fundamental relation should include Baryon TF (BTF) relation SFR-baryon mass relation Kennicutt-Schmidt law as well as other relations. In this talk, we present the result related to 1 and 2.

2. Data Parent data The sample was compiled from previous studies for the baryonic Tully-Fisher relation. To have a large mass (circular velocity) range, we used the following three samples. Then, the sample is heterogeneous. • McGaugh & Wolf (2010) • Dwarf spheroidals • Torres-Flores et al. (2011) • Spirals and irregulars from GHASP (GassendiHAlpha survey of SPirals ) • Gurovich et al. (2010) • Isolated undisturbed spirals

Measurement of SFR The SFR is measured from UV and IR. UV We measured the UV flux from GALEX FUV images (l = 1530Å). The SFR from directly observable UV is obtained by This formula was obtained by Starburst99 model assuming a constant SFR for 108 yr and the Salpeter initial mass function (Salpeter 1955) with a mass range from 0.1M☉ to 100M☉.

Measurement of SFR IR We cross-matched the AKARI point source catalog and quoted fluxes from the data. The SFR hidden by dust is calculated by where h is the fraction of IR luminosity heated by old stars which are not related to the current SFR. Here LTIR stands for the total IR luminosity obtained by the formula of Takeuchi et al. (2010) using the AKARI FIS WIDE-S and WIDE-L:

Measurement of SFR The total SFR is then given by Not all the galaxies in the parent sample have GALEX images or AKARI point source counterpart. The final sample contains 35 galaxies. Redshifts of the sample were obtained from NED, and we assumed h = 0.73, WM0 = 0.24, WL0 = 0.76.

3. Results Baryonic Tully-Fisher relation We obtained a BTF relation from the sample for quite a large circular velocity range. Total baryon mass Mbar [M☉] Circular velocity Vc[kms-1]

3. Results Baryonic Tully-Fisher relation We obtained a BTF relation from the sample for quite a large circular velocity range. We note that even we take into account the stellar and gas mass, we find a downward deviation from a single power law. ⇒ We revisit this issue later. Total baryon mass Mbar [M☉] Circular velocity Vc[kms-1]

Stellar mass-SFR relation (SF main sequence) (r = 0.766) cf. Elbaz et al. (2007) SFR [M☉yr-1] Stellar mass M* [M☉]

Total baryon mass-SFR relation The slope is steeper than the M*-SFR relation. The added gas mass fraction is larger for smaller galaxies, i.e., small galaxies have formed stars slowly, and they have a large gas reservoir. SFR [M☉yr-1] Total Baryon mass Mbar [M☉]

Velocity-total baryon mass-SFR relation

Velocity-total baryon mass-SFR relation We have a non-trivial dependence on both circular velocity and baryon mass.

Velocity-total baryon mass-SFR relation The principal component analysis may be a better tool for this analysis.

4. Discussion HIPASS result The HI Parkes All Sky Survey (HIPASS) team showed This is steeper than the luminosity TF. However, it is still too shallow. Some recent works showed a possible downward deviation from a single power law. Meyer et al. (2008) URL: http://www.atnf.csiro.au/research/multibeam/release/

The “extended” BTF The slope becomes steeper from the largest to the smallest structures (clusters: violet symbols, giant galaxies: blue symbols, and dwarf spheroidals: red symbols). ⇒ Possible effect of feedback? However, gaseous dwarfs are missing on this plot. Toward lower HImasses! McGaugh et al. (2010)

Required sensitivity (for Local galaxies) HI emission: down to HI mass = 103 M☉(~ baryonic mass of dSph) at 3 Mpc. N.B. These galaxies are extended.

Theoretical attempt Trujillo-Gomez et al. (2011) discussed this issue based on LCDM (Bolshoi) + halo abundance matching and HIPASS data. They claim that the velocity-luminosity relation is naturally reproduced simultaneously with correlation functions etc. Trujillo-Gomez et al. (2011)

Theoretical attempt Trujillo-Gomez et al. (2011) discussed this issue based on LCDM (Bolshoi) + halo abundance matching and HIPASS data. They claim that the velocity-luminosity relation is naturally reproduced simultaneously with correlation functions etc. How about SF properties? Trujillo-Gomez et al. (2011)

Star formation properties revisited Surface densities of total gas (HI + H2) and SFR are correlated. We should extend our result to include a galaxy size (radius) to address the issues related to Schmidt-Kennicutt law. To extend the analysis to higher dimensions, the data must be very large (aka the curse of dimension). ⇒ SKA survey! Kennicutt & Evans (2012)

Star formation properties revisited The basic BTF are related mainly to disk galaxies, which have SF activity in general. The general scaling relation includes elliptical galaxies as the Faber-Jackson relation. We note that TF and FJ relations are not the same. The SF galaxies only appears in the SF-related subspace in the multidimensional data-vector space. How to deal?

4. Summary and Prospects Connecting the properties of dark halos and resident galaxies is one of the most fundamental issues in the physics of galaxy formation and evolution. Dynamical properties are explored via TF or FJ relation (velocity-luminosity relation). Some important empirical relations including star-formation properties are known (SF main sequence, Schmidt-Kennicutt law). We constructed a sample of Local galaxies with a large mass range, and found a three-dimensional relation: Some theoretical works seem to succeed in explaining these relations, but still various problems remain unsolved.

4. Summary and Prospects With SKA, we expect various extension and development for this work. Enlarge the sample with a homogeneous selection. For Local sample, the study on the BTF is not very demanding for the performance of the instruments (50 mJy for Local dwarfs). In order to extend it to include the size effect to discuss Schmidt-Kennicutt-type laws, we need a very large sample, but this request will be automatically satisfied. For such a high-dimensional analysis, PCA will be useful. Current theoretical works are based on the HIPASS results. SKA will enables us to much more precise discussions. We can refine the theoretical works. etc., etc…

1. Introduction Halo occupation distribution (HOD) Halo model assumes that the two-point correlation (or power spectrum) of galaxies consists of two components, one-halo and two-halo terms. Peacock (2002)

1. Introduction Halo occupation distribution (HOD) In this framework, the distribution function of the number of galaxies in one halo as a function of the halo mass is referred to as the halo occupation number (HOD). By connecting the HOD (or more precisely, conditional luminosity function) with the halo mass function, we can obtain the galaxy luminosity function. Kravtsov (2003)

Empirical relations including star formation Kennicutt & Evans (2012)

Topics on HI in the Context of Galaxy Evolution: Baryonic Tully Fisher Relation and its Extension