The Evolution of the Tully-Fisher Relation of Spiral Galaxies

Ziegler, B.; Böhm, A.; Fricke, K. J.; Jäger, Klaus; Nicklas, H.; Bender, Ralf; Drory, Niv; Gabasch, A.; Saglia, R. P.; Seitz, S.; Heidt, J.; Mehlert, D.; Möllenhoff, C.; Noll, Stefan; Sutorius, Eckhard

doi:10.1086/338962

Cited by 92 publications

(138 citation statements)

References 29 publications

(14 reference statements)

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“…Pioneer studies, most of them in the B-band, seem to show evolution, although there was no consensus on whether this evolution was on slope, zero point, or both. Ziegler et al (2002) find a shallower relation at high redshift (z = 1) than what has been measured in local samples. In their study, they claim that less massive galaxies were 1 or 2 mag brighter in the past (at fixed rotational velocity), while the most massive would follow the local relation.…”

Section: Introductioncontrasting

confidence: 67%

Evolution of the optical Tully-Fisher relation up to z = 1.3

Lorenzo¹,

Cepa

Bongiovanni³

et al. 2009

A&A

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Context. The study of the evolution of the Tully-Fisher relation has been controversial in the past years. The main difficulty is in determining the required parameters for intermediate and high redshift galaxies, given the cosmological corrections and biases involved. Aims. This work aims to identify the main problems of the study of the Tully-Fisher relation at high redshift using optical emission lines, in order to draw conclusions about the possible evolution of this relation in the B, R, and I-bands. Methods. With this aim, the rotational velocities obtained from the widths of different optical lines using DEEP2 spectra are compared. This method allows reaching higher redshifts against the rotation curve one, due to spatial resolution limitations. Morphology has been determined via HST images, using and comparing different methodologies. Instrumental magnitudes are then corrected for K and extinction and the absolute magnitudes derived for the concordance cosmological model. Finally, the optical Tully-Fisher relations in B, R, and I-bands at different redshifts up to z = 1.3 are derived. Results. Although most studies (this one included) find evidence of evolution, the results are not conclusive enough, since the possible luminosity evolution is within the scattering of the relation, and the evolution in slope is difficult to determine because at high redshift only the brightest galaxies can be measured. Nevertheless, our study shows a clear tendency, which is the same for all bands studied, that favours a luminosity evolution where galaxies were brighter in the past for the same rotation velocity. This result also implies that the colour of the Tully-Fisher relation does not change with redshift, supporting the collapse model versus the accretion model of disc galaxy formation.

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Section: Introductioncontrasting

confidence: 67%

Evolution of the optical Tully-Fisher relation up to z = 1.3

Lorenzo¹,

Cepa

Bongiovanni³

et al. 2009

A&A

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“…The atomic gas masses cover a range from 1.1 × 10 9 M up to 3.8 × 10 10 M with a median mass of the order of 6.2 × 10 9 M . Considering the upper (Schöniger & Sofue 1997;Sakai et al 2000;Ziegler et al 2002). The H i detected sources from this work are coded with grey-scale.…”

Section: Discussionmentioning

confidence: 99%

“…As the inclinations for the sources in this sample are not defined, we can only assume a range of rotation velocities. By inserting graphs for the TullyFisher relation from literature sources (see e.g., Sakai et al 2000;Ziegler et al 2002) we can estimate where our host galaxies should be found in this graph. Since the majority of the 45 • points as well as the value for the median are located to the left of the literature Tully-Fisher functions our objects should feature lower inclination angles of about 30 • , which is in good agreement with our assumption of a nearly face on inclination for low luminosity AGN.…”

Section: Morphologymentioning

confidence: 99%

H I in nearby low-luminosity QSO host galaxies

König¹,

Eckart

García-Marín³

et al. 2009

A&A

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We searched for 21 cm H i emission in a sample of 27 previously CO detected nearby galaxies hosting low-luminosity quasi -stellar objects (QSOs). In this paper we investigate the relationship between the H i and infrared properties of these host galaxies, compare the atomic and molecular gas content and look for connections to the optical and FIR properties. The single dish observations have been made with the Effelsberg 100-m telescope with a beam size of 9.5 . The sample objects have been drawn from a wide-angle survey for optically bright QSOs (HES), which have declinations δ > −30 • and redshifts up to z = 0.06. 12 host galaxies from the sample have been detected in the H i 21 cm emission line. Eight of them have a spiral geometry, whereas the other four are bulge dominated and probably of elliptical type (E/S0). Three of the objects seem to be in a phase of merging/interaction. The neutral atomic gas masses range from 1.1×10 9 M up to 3.8×10 10 M . The median H i gas mass in the whole sample is of the order of 11.4×10 9 M , which is a factor of two higher than the H i content of our galaxy. We find no strong correlation between H i mass and IR luminosity.The objects agree well within the expectations from the Tully-Fisher relation. In the color-color diagram we find all sources in the estimated locations. With the non-detected sources we clearly sample an upper envelope of this mass distribution.

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“…The circular velocities for the late-type galaxies in Table 1 V c have been estimated using the recent results of Ziegler et al (2002), which measure the B-band TF slope and normalization for mag, focal reducer/low dispersion spec-R ! 23 0.5 !…”

Section: The Lensesmentioning

confidence: 99%

“…estimated from the scatter around the best fit in Figure 3 of Ziegler et al (2002). These errors are propagated in the calculation of the Einstein radius, etc., and account for most of the uncertainty in the final value of the magnification.…”

Section: The Lensesmentioning

confidence: 99%

The Magnification of SN 1997[CLC]ff[/CLC], the Farthest Known Supernova

Benı́tez¹,

Riess²,

Nugent³

et al. 2002

The Astrophysical Journal

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With a redshift of , SN 1997ff is the most distant Type Ia supernova (SN Ia) discovered so far. This z ≈ 1.7 SN is close to several bright, galaxies, and we consider the effects of lensing by those objects on z p 0.6-0.9 the magnitude of SN 1997ff. We estimate their velocity dispersions using the Tully-Fisher and Faber-Jackson relations, corrected for evolution effects, and calculate, applying the multiple-plane lensing formalism, that SN 1997ff is magnified by mag. Due to the spatial configuration of the foreground galaxies, the shear 0.34 ‫ע‬ 0.12 from individual lenses partially cancels out, and the total distortion induced on the host galaxy is considerably smaller than that produced by a single lens having the same magnification. After correction for lensing, the revised distance to SN 1997ff is mag, which improves the agreement with the mϪM p 45.49 ‫ע‬ 0.34 Q p M , cosmology expected from lower redshift SNe Ia and which is inconsistent at the ∼3 j confidence 0.35 Q p 0.65 L level with a uniform gray dust model or a simple evolution model.

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The Evolution of the Tully-Fisher Relation of Spiral Galaxies

Cited by 92 publications

References 29 publications

Evolution of the optical Tully-Fisher relation up to z = 1.3

Evolution of the optical Tully-Fisher relation up to z = 1.3

H I in nearby low-luminosity QSO host galaxies

The Magnification of SN 1997[CLC]ff[/CLC], the Farthest Known Supernova

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