The 2MASS Tully-Fisher relation for flat edge-on galaxies

Караченцев, И. Д.; Митронова, С. Н.; Караченцева, В. Е.; Kudrya, Yu. N.; Jarrett, T. H.

doi:10.1051/0004-6361:20021451

Cited by 41 publications

(49 citation statements)

References 22 publications

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“…Verheijen (2001) compared B, R, I and K band luminosities and HI rotation curves and concluded that the TF relation reflects a fundamental correlation between the light and the mass of the dark matter halo. Karachentsev et al (2002) using 2MASS survey data has confirmed this result and found a TF slope increases steadily from the B to K band.…”

Section: Introductionsupporting

confidence: 58%

3D spectroscopy with VLT/GIRAFFE

Flores¹,

Hammer²,

Puech³

et al. 2006

A&A

182

356

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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 < z < 0.75). This facility is able to recover the velocity fields of almost all the emission line galaxies with I AB ≤ 22.5 and W 0 (OII) ≥ 15 Å. 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 Gyr.

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Section: Introductionsupporting

confidence: 58%

3D spectroscopy with VLT/GIRAFFE

Flores¹,

Hammer²,

Puech³

et al. 2006

A&A

182

356

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“…More recently, Tully et al (1998) and Karachentsev et al (2002) have found evidence for an internal extinction law which also depends on rotation velocity. These observations favour a higher amount of absorption in fast rotators than for spirals of low V max .…”

Section: Influence Of the Intrinsic Absorption Correctionmentioning

confidence: 99%

The Tully-Fisher relation at intermediate redshift

Böhm

Ziegler

Saglia

et al. 2004

A&A

111

196

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Abstract. Using the Very Large Telescope in Multi Object Spectroscopy mode, we have observed a sample of 113 field spiral galaxies in the FORS Deep Field (FDF) with redshifts in the range 0.1 < z < 1.0. The galaxies were selected based on apparent brightness (R < 23 m ) and encompass all late spectrophotometric types from Sa to Sdm/Im. Spatially resolved rotation curves have been extracted for 77 galaxies and fitted with synthetic velocity fields taking into account all observational effects from inclination and slit misalignment to seeing and slit width. We also compared different shapes for the intrinsic rotation curve. To obtain robust values of V max , our analysis is focused on galaxies with rotation curves that extend well into the region of constant rotation velocity at large radii. If the slope of the local Tully-Fisher relation (TFR) is held fixed, we find evidence for a mass-dependent luminosity evolution which is as large as up to ∆M B ≈ −2 m for the lowest-mass galaxies, but is small or even negligible for the highest-mass systems in our sample. In effect, the TFR slope is shallower at z ≈ 0.5 in comparison to the local sample. We argue for a mass-dependent evolution of the mass-to-light ratio. An additional population of blue, low-mass spirals does not seem a very appealing explanation. The flatter tilt we find for the distant TFR is in contradiction to the predictions of recent semi-analytic simulations.

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“…Near infrared J, H, K s photometry of galaxies fulfilled in the 2MASS all-sky survey (Jarett et al 2000(Jarett et al , 2003 provides background for constructing TF diagrams for spiral galaxies (Karachentsev et al 2002). Yet, due to short expositions, the 2MASS survey has been found to be undersensitive for detecting low surface brightness objects, especially those ones having blue stellar population.…”

Section: Stellar Tully-fisher Relation For Dwarfsmentioning

confidence: 99%

The Local Tully–fisher Relation for Dwarf Galaxies

Караченцев

Kaisina

Kashibadze

2016

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We study different incarnations of the Tully-Fisher (TF) relation for the Local Volume (LV) galaxies taken from Updated Nearby Galaxy Catalog. The UNGC sample contains 656 galaxies with W 50 HI-line-width estimates, mostly belonging to low mass dwarfs. Of them, 296 objects have distances measured with accuracy better than 10%. For the sample of 331 LV galaxies having baryonic masses log M bar > 5.8 log M ⊙ we obtain a relation log M bar = 2.49 log W 50 + 3.97 with observed scatter of 0.38 dex. The largest factors affecting the scatter are observational errors in K-band magnitudes and W 50 line widths for the tiny dwarfs, as well as uncertainty of their inclinations. We find that accounting for the surface brightness of the LV galaxies, or their gas fraction, or specific star formation rate, or the isolation index do not reduce essentially the observed scatter on the baryonic TF-diagram. We also notice that a sample of 71 dSph satellites of the Milky Way and M31 with known stellar velocity dispersion σ * tends to follow nearly the same bTF relation, having slightly lower masses than that of late-type dwarfs.

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The 2MASS Tully-Fisher relation for flat edge-on galaxies

Cited by 41 publications

References 22 publications

3D spectroscopy with VLT/GIRAFFE

3D spectroscopy with VLT/GIRAFFE

The Tully-Fisher relation at intermediate redshift

The Local Tully–fisher Relation for Dwarf Galaxies

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