THE SINS SURVEY: MODELING THE DYNAMICS OF z ∼ 2 GALAXIES AND THE HIGH-z TULLY–FISHER RELATION

By G. Cresci, E. Hicks, R. Genzel, N. F. Förster Schreiber, Roger Davies, N. Bouché, P. Buschkamp, Shy Genel, K. Shapiro, L. Tacconi and 16 more. 2009

222 citations recorded by the source corpus.

We present the modeling of SINFONI integral field dynamics of 18 star-forming galaxies at z ∼ 2 from Hα line emission. The galaxies are selected from the larger sample of the SINS survey, based on the prominence of ordered rotational motions with respect to more complex merger-induced dynamics. The quality of the data allows us to carefully select systems with kinematics dominated by rotation, and to model the gas dynamics across the whole galaxy using suitable exponential disk models. We obtain a good correlation between the dynamical mass and the stellar mass, finding that large gas fractions (Mgas ≈ M*) are required to explain the difference between the two quantities. We use the derived stellar mass and maximum rotational velocity Vmax from the modeling to construct for the first time the stellar mass Tully–Fisher relation at z ∼ 2.2. The relation obtained shows a slope similar to what is observed at lower redshift, but we detect an evolution of the zero point. We find that at z ∼ 2.2 there is an offset in log(M*) for a given rotational velocity of 0.41 ± 0.11 with respect to the local universe. This result is consistent with the predictions of the latest N-body/hydrodynamical simulations of disk formation and evolution, which invoke gas accretion onto the forming disk in filaments and cooling flows. This scenario is in agreement with other dynamical evidence from SINS, where gas accretion from the halo is required to reproduce the observed properties of a large fraction of the z ∼ 2 galaxies.

Subfields: Astronomy and Astrophysics, Instrumentation

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In Astronomy and Astrophysics

1. P. Hopkins
2. L. Hernquist
3. R. Dav'e
4. R. Somerville
5. A. Dekel
6. T. Naab
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In Instrumentation

1. P. Hopkins
2. L. Hernquist
3. A. Dekel
4. R. Dav'e
5. R. Somerville
6. P. V. van Dokkum
7. Thomas J. Cox
8. T. Naab

Citations in the corpus

• A UNIVERSAL, LOCAL STAR FORMATION LAW IN GALACTIC CLOUDS, NEARBY GALAXIES, HIGH-REDSHIFT DISKS, AND STARBURSTS (2011, unknown): “In the other direction, in high redshift disks the scale height is not directly measured, but is likely to be large since the gas velocity dispersion is ∼ 50 km s−1 (Cresci et al. 2009), a factor of ∼ 6 larger than the typical value in local disk galaxies.”
• Discriminating Between the Physical Processes that Drive Spheroid Size Evolution (2009, result): “At z = 2, direct measurements are not always available; the gas masses from Erb et al. (2006) are estimated indirectly based on the observed surface densities of star formation and assuming that the z = 0 Kennicutt law holds; other indirect estimates yield similar results (Cresci et al. 2009).”
• CONSTRAINTS ON THE ASSEMBLY AND DYNAMICS OF GALAXIES. I. DETAILED REST-FRAME OPTICAL MORPHOLOGIES ON KILOPARSEC SCALE OF z ∼ 2 STAR-FORMING GALAXIES (2010, methodology): “′′20 resolution (Shapiro et al. 2008; Genzel et al. 2008; Förster Schreiber et al. 2009; Genzel et al. 2010; P. Buschkamp et al. 2011, in preparation).”
• THE KMOS3D SURVEY: DESIGN, FIRST RESULTS, AND THE EVOLUTION OF GALAXY KINEMATICS FROM 0.7 ⩽ z ⩽ 2.7 (2014, methodology): “Additionally, we fit the approximation for the velocity dispersion in a thick disk (σ02; Genzel et al. 2008; Cresci et al. 2009) to the dispersion profile with a constant level of intrinsic dispersion, σ01, added in quadrature as described by; σ02(r) = vrot(r)hz r , (A2) σmod(r) = √ σ201 + σ02(r) 2.”
• Ionized gas outflows and global kinematics of low-z luminous star-forming galaxies (2014, methodology): “…by combining a large amount of data for SFGs at z∼ 1.5-3 obtained by several authors (Forster-Schreiber et al. 2006, 2009; Genzel et al. 2006, 2008; Cresci et al. 2009; Wright et al. 2007; Starkenburg et al 2009; Epinat et al. 2009; LemoineBusserolle & Lamareille 2010; Law et al. 2009; Jones et…”
• Feedback-regulated star formation in molecular clouds and galactic discs (2013, background): “…(z ∼ 2) starforming galaxies have comparably large gas fractions (e.g., Daddi et al. 2010b; Tacconi et al. 2010) and are also inferred to have velocity dispersions that are elevated (Cresci et al. 2009; Genzel et al. 2011) relative to local spirals, which have cT ≈ 10 km s−1 (Dib et al. 2006).”
• Rotational support of giant clumps in high-z disc galaxies (2011, result): “As shown in CDB10, galaxies A-C are consistent with the observed scaling relations ofz ∼ 2 galaxies, including the relation between SFR and stellar mass and the Tully-Fisher relation (Förster Schreiber et al. 2009; Cresci et al. 2009).”
• The multi-phase winds of Markarian 231: from the hot, nuclear, ultra-fast wind to the galaxy-scale, molecular outflow (2015, result): “Following Cresci et al. (2009), the adopted surface brightness profile for both components is exponential I(r) = I0 e−r/r0 (2) The disk model and fit results are shown in Fig.”
• EVOLVING GRAVITATIONALLY UNSTABLE DISKS OVER COSMIC TIME: IMPLICATIONS FOR THICK DISK FORMATION (2011, background): “…are dominated by large luminous clumps of gas (Elmegreen et al. 2004, 2005; Förster Schreiber et al. 2009), while measurements of the velocity dispersion of such massive star-forming galaxies have found values near 50 km/s spread across the entire disk (Cresci et al. 2009; Genzel et al. 2011).”
• How Stellar Feedback Simultaneously Regulates Star Formation and Drives Outflows (2015, background): “…a theoretically motivated functional form (Kereš et al. 2005, 2009) to a compilation of observations (Bell & de Jong 2000; McGaugh 2005; Shapley et al. 2005; Erb et al. 2006b; Erb 2008; Calura et al. 2008; Puech et al. 2008; Cresci et al. 2009; Förster Schreiber et al. 2009; Mannucci et al. 2009).”
• THE IMPACT OF COLD GAS ACCRETION ABOVE A MASS FLOOR ON GALAXY SCALING RELATIONS (2009, background): “The TF relation appears to be already in place at high-redshifts z ≥ 1 (Kassin et al. 2007; Puech et al. 2008; Epinat et al. 2009; Cresci et al. 2009) and has evolved by a factor of 2.5 at a given mass (Cresci et al. 2009) from z ≃ 2.2 to the present.”
• High-redshift clumpy discs and bulges in cosmological simulations (2009, methodology): “The observational data are taken from the SINS sample of disc galaxies (Cresci et al. 2009).”
• THE EPOCH OF DISK SETTLING: z ∼ 1 TO NOW (2012, methodology): “For galaxies at z ∼ 2, data are adopted from the SINS Survey via private communication from N. FörsterSchreiber for the most recent models and data as of August 2011 for galaxies in Genzel et al. (2008), FörsterSchreiber et al. (2009), and Cresci et al. (2009).”
• The effects of gas on morphological transformation in mergers: implications for bulge and disc demographics (2009, result): “At z = 2, direct measurements are not available; the gas masses from Erb et al. (2006) are estimated indirectly based on the observed surface densities of star formation and assuming that the z = 0 Kennicutt law holds; other indirect estimates yield similar results (Cresci et al. 2009).”
• Resolved spectroscopy of gravitationally lensed galaxies: recovering coherent velocity fields in subluminous z ~ 2-3 galaxies (2009, methodology): “…the five lensed galaxies which are reasonably well fit by disk models compared to the compact LBGs from Law et al. (2009) and the rotationdominated SINS galaxies described by Cresci et al. (2009), showing that the ratio of velocity shear to dispersion is higher for larger, more massive galaxies.”
• MERGERS AND BULGE FORMATION IN ΛCDM: WHICH MERGERS MATTER? (2009, background): “However other observations suggest that it does indeed hold (Bouché et al. 2007), and other indirect estimates yield similar results (Cresci et al. 2009; Mannucci et al. 2009).”
• Evidence for strong dynamical evolution in disc galaxies through the last 11 Gyr. GHASP VIII – a local reference sample of rotating disc galaxies for high‐redshift studies (2009, methodology): “…used for such studies in the literature and which may have rising, flat or decreasing shape: (1) an exponential disk as used for the SINS sample (Cresci et al. 2009); (2) an isothermal sphere as used in mass models (Spano et al. 2008); (3) a model described by an inner linear slope to reach Vt…”