3D spectroscopy with VLT/GIRAFFE. I. The true Tully Fisher relationship at z ̃ 0.6

By H. Flores, F. Hammer, M. Puech, P. Amram, C. Balkowski. 2006

137 citations recorded by the source corpus.

A precise derivation of the evolution of the Tully Fisher is crucial to understand the interplay between dark matter and baryonic matter in cosmological models, Using 15 deployable integral field units of FLAMES/GIRAFFE at VLT, we have recovered the velocity fields of 35 galaxies at intermediate redshift (0.4 =15A In our sample, we find only 35% rotating disks. These rotating disks produce a Tully-Fisher relationship (stellar mass or M_K versus V_max) which has apparently not evolved in slope, zero point and scatter since z=0.6. The only evolution found is a brightening of the B band luminosity of a third of the disks, possibly due to an enhancement of the star formation. The very large scatters found in previously reported Tully-Fisher relationships at moderate redshifts are caused by the numerous (65%) galaxies with perturbed or complex kinematics. Those galaxies include minor or major mergers, merger remnants and/or inflow/outflows and their kinematics can be easily misidentified by slit spectroscopy. Their presence suggests a strong evolution in the dynamical properties of galaxies during the last 7 Gyrs.

Subfields: Astronomy and Astrophysics, Instrumentation

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In Astronomy and Astrophysics

1. P. Hopkins
2. L. Hernquist
3. Thomas J. Cox
4. R. Somerville
5. A. Dekel
6. R. Dav'e
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In Instrumentation

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

Citations in the corpus

• The Stellar Mass Tully-Fisher Relation to z = 1.2 from AEGIS (2006, background): “Distant stellar-mass TFRs (M∗TFRs) have also been studied (Conselice et al. 2005; Flores et al. 2006).”
• 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): “To conclude, the kinematical classification made by Flores et al. (2006) is relevant for a reasonable fraction of rotating disks, assuming that the local velocity dispersion is lower than the rotation velocity.”
• A Theoretical Interpretation of the Black Hole Fundamental Plane (2007, background): “If the baryonic Tully-Fisher relation does not evolve with redshift, as suggested by observations (Conselice et al. 2005; Flores et al. 2006) – i.e.the kinematic structure of disks does not strongly evolve, then we haveMtot ∝ v4disk (Bell & de Jong 2001; McGaugh 2005, vdisk being the disk circular…”
• DISSIPATION AND EXTRA LIGHT IN GALACTIC NUCLEI. IV. EVOLUTION IN THE SCALING RELATIONS OF SPHEROIDS (2008, methodology): “This is also reflected in e.g. the baryonic Tully-Fisher relation, which appears to evolve negligibly from z = 0− 2 (Conselice et al. 2005; Flores et al. 2006; Kassin et al. 2007; van Dokkum et al. 2004).”
• The KMOS Redshift One Spectroscopic Survey (KROSS):dynamical properties, gas and dark matter fractions of typical z~1 star-forming galaxies (2016, unknown): “The Tully–Fisher relation (Tully & Fisher 1977) is also found to evolve for galaxies at progressively high redshifts (although see Flores et al. 2006), in that galaxies with the same rotation velocity in the distant Universe have lower stellar masses (e.g. Swinbank et al. 2006).”
• CONSTRAINTS ON THE ASSEMBLY AND DYNAMICS OF GALAXIES. I. DETAILED REST-FRAME OPTICAL MORPHOLOGIES ON KILOPARSEC SCALE OF z ∼ 2 STAR-FORMING GALAXIES (2010, background): “…between disks and mergers as a function of the degree of symmetry of velocity fields and velocity dispersion maps (e.g., Krajnovíc et al. 2006; Flores et al. 2006; Shapiro et al. 2008; Épinat et al. 2010), and to determine the main source of dynamical support from the ratio of rotation…”
• MERGERS AND BULGE FORMATION IN ΛCDM: WHICH MERGERS MATTER? (2009, background): “…of high redshift disk+bulge systems that may represent recent re-forming or relaxing merger remnants can constrain the efficiency of bulge formation in mergers (Hammer et al. 2005; Zheng et al. 2005; Trujillo & Pohlen 2005; Flores et al. 2006; Puech et al. 2007a,b, 2008; Atkinson et al. 2007).”
• THE EPOCH OF DISK SETTLING: z ∼ 1 TO NOW (2012, methodology): “Similarly, from samples of 33 and 68 galaxies in the IMAGES Survey at z ∼ 0.6, Flores et al. (2006) and Yang et al. (2008), respectively, found a large scatter in the TFR due to galaxies with “perturbed or complex kinematics.””
• Dissipation and Extra Light in Galactic Nuclei. I. Gas-Rich Merger Remnants (2008, methodology): “Likewise, we obtain the fits to the observed surface brightness profiles in Figures 6–11 given progenitor disks that obey the baryonic TullyFisher and size–stellar mass relations (observed to evolve only weakly from z ¼ 0 1; e.g., Bell & de Jong 2001; Flores et al. 2006; Trujillo et al. 2006).”
• The effects of gas on morphological transformation in mergers: implications for bulge and disc demographics (2009, background): “These processes, it appears, are now being seen in a growing number of observations (Hammer et al. 2005; Trujillo & Pohlen 2005; Zheng et al. 2005; Flores et al. 2006; Puech et al. 2007a,b; Atkinson, Conselice & Fox 2007; Puech et al. 2008).”
• A Cosmological Framework for the Co-Evolution of Quasars, Supermassive Black Holes, and Elliptical Galaxies. II. Formation of Red Ellipticals (2007, result): “…we assume does not evolve with redshift (as suggested by a large number of observations at least to z 1:5, and by some to zk 3; Conselice et al. 2005; Flores et al. 2006; Bell et al. 2006b; Kassin et al. 2007; van Dokkum et al. 2004), but we have tried all three estimators and find similar results.”
• HOW DO DISKS SURVIVE MERGERS? (2008, background): “With increasing redshift, kinematic and morphological indications of recent, violent disturbance in disk-dominated galaxies appear more frequent (Hammer et al. 2005; Flores et al. 2006; Puech et al. 2007, 2008).”
• THE SINS SURVEY: MODELING THE DYNAMICS OF z ∼ 2 GALAXIES AND THE HIGH-z TULLY–FISHER RELATION (2009, background): “The differences with the results obtained by Flores et al. (2006) on a similar dataset are attributed to both a difference in the reference local relation and a more accurate measurement of the rotation velocity at high redshift.”
• Integral field spectroscopy with SINFONI of VVDS galaxies I. Galaxy dynamics and mass assembly at 1.2 < z < 1.6 (2009, methodology): “…large sample of galaxies (more than∼50 galaxies), high redshift TFR were derived from long-slit spectroscopy samples, except the ones derived by (i) Flores et al. (2006) and Puech et al. (2008) from FLAMES/GIRAFFE IFUs data atz ∼ 0.6; (ii) Cresci et al. (2009) from SINFONI data atz ∼ 2.2 and…”
• VLT/VIMOS integral field spectroscopy of luminous and ultraluminous infrared galaxies: 2D kinematic properties (2013, unknown): “This classification is similar to the one proposed by Flores et al. (2006) and distinguishes three main groups: 1.”
• The Tully-Fisher relations of early-type spiral and S0 galaxies (2010, background): “Conselice et al. (2005), Flores et al. (2006) and Kassin et al. (2007) find no evidence for evolution in either the slope or zeropoint of the K-band spiral TFR from the local universe to z ≈ 1.”