The redshift evolution of the Tully-Fisher Relation probes gravitational dynamics that must be consistent with any modified gravity theory seeking to explain the galactic rotation curves without the need for dark matter. Within the context of non-relativistic Modified Newtonian Dynamics (MOND), the characteristic acceleration scale of the theory appears to be related to the current value of either the Hubble constant, i.e., alpha ~ cH_0, or the dark energy density, i.e., alpha (8 pi G rho_lambda/3)^{1/2}. If these relations are the manifestation of a fundamental coupling of a_0 to either of the two cosmological parameters, the cosmological evolution would then dictate a particular dependence of the MOND acceleration scale with redshift that can be tested with Tully-Fisher relations of high-redshift galaxies. We compare this prediction to two sets of Tully-Fisher data with redshifts up to z=1.2. We find that both couplings are excluded within the formal uncertainties. However, when we take into account the potential systematic uncertainties in the data, we find that they marginally favor the coupling of the MOND acceleration scale to the density of dark energy.
This paper explores the adherence of 47 extreme late-type galaxies to the B- and V-band Tully-Fisher relations defined by a sample of local calibrators. In both bands we find the mean luminosity at a given line width for extreme late-type spirals to lie below that predicted by standard Tully-Fisher relations. While many of the extreme late-type spirals do follow the Tully-Fisher relation to within our observational uncertainties, most of these galaxies lie below the normal, linear Tully-Fisher relation, and some are underluminous by more than 2 sigma (i.e. >1.16 magnitudes in V). This suggests…
The Tully-Fisher relationship is subject to morphological type dependence such that galaxies of morphology similar to ScI galaxies and Seyfert galaxies are more luminous at a given rotational velocity than galaxies of other morphological classification. This effect is most prevalent in the B-band. It is shown that the type effect is not simply an artifact of the calibrator sample, but is also present in cluster samples. The type effect is corrected by creating type dependent Tully-Fisher relations for ScI group galaxies and Sb/ScIII group galaxies. It is shown that with single calibrations, th…
We update and extend the results of Shanks (1997, MNRAS, 290, L77) by making a direct test of Tully-Fisher distance estimates to thirteen spiral galaxies with HST Cepheid distances and to ten spiral galaxies with Type Ia supernova (SNIa) distances. The results show that the Tully-Fisher distance moduli are too short with respect to the Cepheid distances by 0.46+-0.11mag and too short with respect to the SNIa distances by 0.49+-0.18mag. Combining the HST Cepheid and the best SNIa data suggests that, overall, previous Tully-Fisher distances at v~1000 kms-1 were too short by 0.43+-0.09mag, a resu…
We explore the Tully-Fisher relation over five decades in stellar mass in galaxies with circular velocities ranging over 30 < Vc < 300 km/s. We find a clear break in the optical Tully-Fisher relation: field galaxies with Vc < 90 km/s fall below the relation defined by brighter galaxies. These faint galaxies are however very gas rich; adding in the gas mass and plotting baryonic disk mass Md = M* + Mg in place of luminosity restores a single linear relation. The Tully-Fisher relation thus appears fundamentally to be a relation between rotation velocity and total baryonic mass of the form Md = A…
We make a direct test of Tully-Fisher distance estimates to eleven spiral galaxies with HST Cepheid distances and to twelve spiral galaxies with SNIa distances. The HST Cepheid distances come from the work of Freedman (1997), Sandage et al (1996) and Tanvir et al (1995). The SNIa distances come from Pierce (1994), calibrated using the Cepheid results of Sandage et al (1996). The Tully-Fisher distances mostly come from the work of Pierce (1994). The results show that the Tully-Fisher distance moduli are too short with respect to the Cepheid distances by 0.46+-0.14mag and too short with respect …
We investigate effects of galaxy-galaxy interaction on the Tully-Fisher relation. The HI linewidth in interacting galaxies is significantly broader than the CO linewidth, and the HI to CO linewidth ratio is proportional to the strength of interaction. This provides different distances to galaxies measured by the Tully-Fisher relation with the CO and HI linewidths. Distances derived from the HI linewidths are 62% larger than those derived from the CO linewidths for strongly interacting galaxies, and 25% larger for weakly interacting galaxies. We argue that the CO-line Tully-Fisher relation will…
As a basic step for establishing the CO-line Tully-Fisher relation for distant galaxies, we made a comparative study of HI versus CO line profiles. Total line profiles of the CO line emission from 32 galaxies have been compared with the corresponding HI emission. We found a good correlation between the profiles of CO and HI. This strongly supports the thesis that CO can be used in the Tully-Fisher relation for distant galaxies where HI observations cannot reach. We also argue that CO can be used as an alternative to HI for un-isolated galaxies such as those in dense cluster of galaxies. Using …
In this brief contribution, I outline hopes of understanding the origin of galaxy scaling relations using numerical simulations as a tool to gain understanding. The case of the Tully--Fisher relation for disk galaxies is used as an example to illustrate the modest achievements to date and the difficult tasks ahead.
A comparison between the CO and HI Tully-Fisher relation for a sample of 30 Virgo ga\-la\-xies shows no significant difference concerning the intrinsic scatter. The distance moduli from both relations after correcting for the sample incompleteness bias agree within the errors and also show no significant difference with previous studies of the Virgo cluster using a complete sample. The CO total linewidth and the CO flux were found to be not well correlated. However, if the distances to the individual galaxies were calculated by the CO Tully-Fisher relation, the CO luminosities calculated using…
We present Tully-Fisher observations for 35 rich Abell clusters of galaxies. Results from I band photometry and optical rotation curve work comprise the bulk of this paper. This is the third such data installment of an all-sky survey of 52 clusters in the distance range 50 to 200\h Mpc. The complete data set provides the basis for determining an accurate Tully-Fisher template relation and for estimating the amplitude and direction of the local bulk flow on a 100\h Mpc scale.
A number of observations strongly suggest that the baryon fraction is not a universal constant. One obvious interpretation is that there is some distribution of Fb, and the different observations sample different portions of the distribution. However, the small intrinsic scatter in the Tully-Fisher relation requires that the baryon fraction be very nearly universal. It is not easy to resolve this paradox in the framework of the standard picture.
We have studied the relation between HI linewidth and optical luminosity in two samples of dwarf galaxies, with special attention to the accuracy of the inclination correction. The first sample consists of rotationally supported galaxies, and has DDO 154 as a prototype. They have HI linewidths significantly larger than predicted by an extrapolation of the Tully-Fisher relation. The deviation from the extrapolated Tully-Fisher relation correlates with the distance-independent mass-to-luminosity ratio M_HI/L_B. The baryonic correction for these gas rich galaxies is too small to explain the devia…
A new technique for calibrating Tully-Fisher like relations by using field galaxies is proposed. Based on a null-correlation approach (NCA), the technique is insensitive to the presence of selection effects on apparent magnitude $m$ and on log line-width distance indicator $p$. This interesting property is used for discarding near by galaxies of the observed sample. It is shown that such a subsampling allows in effect to attenuate biases on calibration parameters created by the presence of radial peculiar velocities.
We present an updated estimate of the surface density and surface brightness in B,V,I of the local Galactic disc, based on a model for the "Solar cylinder" calibrated to reproduce Hipparcos and Tycho star counts. We discuss the mass-to-light ratio of the local stellar disc and infer the global luminosity of the Milky Way, which results underluminous with respect to the Tully-Fisher relation.
We show that the Tully-Fisher relation observed for spiral galaxies can be explained in the current scenario of galaxy formation without invoking subtle assumptions, provided that galactic-sized dark haloes have shallow, core-like central profiles, with a core radius proportional to halo circular velocity. In such a system, both disk and halo contribute significantly to the maximum rotation of the disk, and the interaction between the disk and halo components acts to reduce the scatter in the Tully-Fisher relation. With model parameters chosen in plausible ranges, the model can well accommodat…
A correlation between (1) the difference between the Tully-Fisher calculated distance and Cepheid calculated distance for a target galaxy and (2) the magnitude and distance of galaxies close to the target galaxy is described. The result is based on a sample of 31 galaxies that have published Cepheid distances with a wide range of characteristics and distances from 2.02 Mpc to 49.7 Mpc. The energy impinging on a target galaxy from neighboring galaxies is related to the residual between Tully-Fisher and Cepheid distance calculations of the target galaxy. These relations have four different zones…
In a previous paper, we have demonstrated the importance to define a statistical model describing the observed linear correlation between the absolute magnitude $M$ and the log line width distance indicator $p$ of galaxies (the Tully-Fisher relation). As long as the same statistical model is used during the calibration step of the relation and the step of the determination of the distances of galaxies, standard statistical methods such as the maximum likelihood technic permits us to derive bias free estimators of the distances of galaxies. However in practice, it is convenient to use a differe…
We find a new Tully-Fisher-like relation for spiral galaxies holding at different galactocentric radii. This Radial Tully-Fisher (RTF) relation allows us to investigate the distribution of matter in the optical regions of spiral galaxies. This relation, applied to three different samples of rotation curves of spiral galaxies, directly proves that: 1) the rotation velocity of spirals is a good measure of their gravitational potential and both the RC's amplitudes and profiles are well predicted by galaxy luminosity 2) the existence of a dark component, less concentrated than the luminous one, an…
We have previously demonstrated that Tully-Fisher residuals correlate with tracers of star formation history (color and emission line equivalent width) for a broad sample of Sa--Sd spiral galaxies (Kannappan, Fabricant, & Franx 2002). Here we use these correlations to study two other classes of galaxies: (1) galaxies in close pairs and (2) galaxies at intermediate redshift.
We present new magnitudes derived from 1.65 micron images for 23 galaxies in the Ursa Major cluster. Magnitudes now exist for all but one spiral meeting our criteria for cluster membership and having HI velocity width greater than 187 km/s and inclination greater than 45 deg. These spirals fit a Tully-Fisher relation with dispersion in intrinsic magnitudes (after known observational uncertainties and the effect of cluster depth are removed) of 0.36 and a slope of 10.2 +/- 0.6. The magnitude dispersion is smaller than found in the Virgo cluster but still significantly larger than claimed by som…
I describe the disk mass-rotation velocity relation which underpins the familiar luminosity-linewidth relation. Continuity of this relation favors nearly maximal stellar mass-to-light ratios. This contradicts the low mass-to-light ratios implied by the lack of surface brightness dependence in the same relation.
New models for the formation of disk galaxies are presented. I discuss the contraints on galaxy formation that follow from fitting the model to the near-infrared Tully-Fisher (TF) relation, with an emphasis on reproducing the small amount of scatter observed. Once the parameters that describe the supernova feedback are tuned to fit the slope of the observed TF relation, the model reproduces the correct amount of TF scatter, and yields gas mass fractions, mass-to-light ratios, and characteristic accelerations that are all in excellent agreement with observations.
We study the locus of dwarf and giant early and late-type galaxies on the Tully-Fisher relation (TFR), the stellar mass Tully-Fisher relation (sTFR) and the so-called baryonic or HI gas+stellar mass Tully-Fisher relation (gsTFR). We show that early-type and late-type galaxies, from dwarfs to giants, trace different yet approximately parallel TFRs. Surprisingly, early-type and late-type galaxies trace a single yet curved sTFR over a range of 3.5 orders of magnitude in stellar mass. Moreover, all galaxies trace a single, linear gsTFR, over 3.5 orders of magnitude in HI gas+stellar mass. Dwarf el…
We present the B band Tully-Fisher relation for Low Surface Brightness (LSB) galaxies. These LSB galaxies follow the same Tully-Fisher relation as normal spiral galaxies. This implies that the mass-to-light ratio (M/L) of LSB galaxies is typically a factor of 2 larger than that of normal galaxies of the same total luminosity and morphological type. Since the dynamical mass of a galaxy is related to the rotation velocity and scale length via M \propto V^2 h, at fixed linewidth LSB galaxies must be twice as large as normal galaxies. This is confirmed by examining the relation between scale lengt…
We use Monte Carlo realizations of halo formation histories and a spherical accretion model to calculate the expected scatter in the velocity dispersions of galactic halos of a given mass due to differences in their formation times. Assuming that the rotational velocity of a spiral galaxy is determined by the velocity dispersion of its halo and that its luminosity is related to its total baryonic mass, this scatter translates to a minimum intrinsic scatter in the Tully-Fisher relation. For popular cosmological models we find that the scatter due to variations in formation histories is by itsel…
A long standing problem for hierarchical disk galaxy formation models has been the simultaneous matching of the zero point of the Tully-Fisher relation and the galaxy luminosity function (LF). We illustrate this problem for a typical disk galaxy and discuss three solutions: low stellar mass-to-light ratios, low initial dark halo concentrations, and no halo contraction. We speculate that halo contraction may be reversed through a combination of mass ejection through feedback and angular momentum exchange brought about by dynamical friction between baryons and dark matter during the disk formati…
We have determined distances and Hubble ratios for galaxies at intermediate redshifts, cz=about 10,000 to 35,000 km/s, by applying the CO-line Tully-Fisher relation to our 12CO (J=1-0)-line observations using the Nobeyama 45-m telescope, and near-IR (NIR) photometry in the J and H bands using the 1.88-m telescope at Okayama Astrophysical Observatory. By averaging the Hubble ratios from J-band result, we obtain a Hubble constant of H_0 = 60 (+/- 10) km/s/Mpc. We argue that the CO line-NIR TFR can be a complimentary method to the other methods for measuring distances of galaxies at intermediate …
Aims. We attempt to determine the optical depth of spiral galaxy disks by a statistical study of new Tully-Fisher data from the ongoing KLUN+ survey, and to clarify the difference between the true and apparent behavior of optical depth. Methods. By utilizing so-called normalized distances, a subsample of the data is identified to be as free from selection effects as possible. For these galaxies, a set of apparent quantities are calculated for face-on positions using the Tully-Fisher diameter and magnitude relations. These values are compared with direct observations to determine the mean value…
We propose and show that the dependence of the internal face-on dust absorption upon B-band luminosity reported by Wang & Heckman (1996) for a sample of late-type galaxies may explain the empirical color-magnitude and color Tully-Fisher relations of disk galaxies. Thus, in order to explain these relations, it is not necessary to evoke star formation and gas infall efficiencies dependent on the mass of the galaxy system. After applying the Wang & Heckman's luminosity-dependent extinction to hierarchical inside-out galaxy formation and evolution models where the star formation and gas infall eff…
Calibrated Tully-Fisher relations ''absolute magnitude - HI line width'' for spiral galaxies oriented edge-on are derived from published data. The slope of the linear fits, especially in R- and I- bands, is close to the value of -10, as predicted by the theory. The standard errors of the relations in B, V, R and I bands are 0.40, 0.36, 0.31 and 0.34 mag, corresponding to relative distance errors of 18%, 17%, 14% and 16%, respectively. The magnitude of an edge-on galaxy appears to be a good distance indicator.
We present the first determination of the Tully-Fisher relation (TFR) for a distant galaxy cluster. We have measured internal kinematics of seven members of Cl0024+1654 from spatially resolved emission observed in 2D Keck (LRIS) spectra. Measurements of disk structural parameters were made from HST (WFPC2) images. While we do not find evidence for a change in the slope or zeropoint of the cluster TFR, we do find that there was more scatter in the past. We intend to expand this study with kinematic measurements from fifteen more Cl0024 members.
We use optical rotation curves to investigate the R-band Tully-Fisher properties of a sample of 90 spiral galaxies in close pairs. The galaxies follow the Tully-Fisher relation remarkably well, with the exception of eight distinct 3-sigma outliers. Although most of the outliers show signs of recent star formation, gasdynamical effects are probably the dominant cause of their anomalous Tully-Fisher properties. Four outliers with small emission line widths have very centrally concentrated line emission and truncated rotation curves; the central emission indicates recent gas infall after a close …
We analyze residuals from the Tully-Fisher relation for the emission-line galaxies in the Nearby Field Galaxy Survey, a broadly representative survey designed to fairly sample the variety of galaxy morphologies and environments in the local universe. For spirals brighter than M_R^i=-18, we find strong correlations between Tully-Fisher residuals and both B-R color and EW(Halpha). The extremes of the correlations are populated by Sa galaxies, which show consistently red colors, and spirals with morphological peculiarities, which are often blue. If we apply an EW(Halpha)-dependent or B-R color-de…
We present the rest-frame B-band Tully-Fisher relation for a sample of 8 cluster spiral galaxies at z = 0.83 and 19 field spirals at z = 0.15-0.90 based on VLT spectroscopy and HST photometry. No strong difference is detected between the cluster and the field galaxies, but we find some evidence that the cluster spirals are ~0.5-1 mag brighter than the field ones at a fixed rotation velocity. Although only a ~1.5-2 sigma result, if confirmed with larger samples this effect could be due to the cluster spirals experiencing a period of enhanced star formation while falling into the cluster.
We have investigated the Tully-Fisher relation for Polar Ring Galaxies (PRGs), based on near infrared, optical and HI data available for a sample of these peculiar objects. Many PRGs show larger HI line-widths than expected for the observed K band luminosity, and this result is confirmed by a larger sample of objects, based on B-band data. This observational evidence may be related to the dark halo shape and orientation in these systems: the larger rotation velocities observed in PRGs can be explained by a flattened polar halo, aligned with the polar ring.
The use of the Tully-Fisher (TF) relation for the determination of the Hubble Constant relies on the availability of an adequate template TF relation and of reliable primary distances. Here we use a TF template relation with the best available kinematical zero-point, obtained from a sample of 24 clusters of galaxies extending to cz ~ 9,000 km/s, and the most recent set of Cepheid distances for galaxies fit for TF use. The combination of these two ingredients yields H_not = 69+/-5 km/(s Mpc). The approach is significantly more accurate than the more common application with single cluster (e.g. …
We study the location of massive disk galaxies on the Tully-Fisher relation. Using a combination of K-band photometry and high-quality rotation curves, we show that in traditional formulations of the TF relation (using the width of the global HI profile or the maximum rotation velocity), galaxies with rotation velocities larger than 200 km/s lie systematically to the right of the relation defined by less massive systems, causing a characteristic `kink' in the relations. Massive, early-type disk galaxies in particular have a large offset, up to 1.5 magnitudes, from the main relation defined by …
The application of the I band Tully--Fisher relation towards determining the Hubble constant is reviewed, with particular attention to the impact of scatter and bias corrections in the relation. A template relation is derived from galaxies in 24 clusters. A subset of 14 clusters with cz ~ 4000 to 9000 km/s is used as an inertial frame to define the velocity zero point of the relation. Twelve galaxies with Cepheid distances are used to establish the absolute magnitude scale of the Tully--Fisher relation, and thus to determine a value of H_not = 70\pm5 km/s/Mpc. Estimates of the peculiar velocit…
We have investigated the Tully-Fisher relation for Polar Ring Galaxies (PRGs), based on near infrared, optical and HI data available for a sample of these peculiar objects. The total K-band luminosity, which mainly comes from the central host galaxy, and the measured HI linewidth at 20% of the peak line flux density, which traces the potential in the polar plane, place most polar rings of the sample far from the Tully-Fisher relation defined for spiral galaxies, with many PRGs showing larger HI linewidths than expected for the observed K band luminosity. This result is confirmed by a larger sa…
The Tully-Fisher Relation (TFR) links two fundamental properties of disk galaxies: their luminosity and their rotation velocity (mass). The pioneering work of Vogt et al. in the 1990's showed that it is possible to study the TFR for spiral galaxies at considerable look-back-times, and use it as a powerful probe of their evolution. In recent years, several groups have studied the TFR for galaxies in different environments reaching redshifts beyond one. In this brief review I summarise the main results of some of these studies and their consequences for our understanding of the formation and evo…
We construct the first "face-on" Tully-Fisher (TF) relation for 24 galaxies with inclinations between 16 degrees and 41 degrees. The enabling measurements are integral-field, echelle spectroscopy from the WIYN 3.5m telescope, which yield accurate kinematic estimates of disk inclination to 15 degrees. Kinematic inclinations are of sufficient accuracy that our measured TF scatter of 0.42 mag is comparable to other surveys even without internal-absorption corrections. Three of four galaxies with significant kinematic and photometric asymmetries also have the largest deviations from our TF relatio…
This paper presents 452 new 21-cm neutral hydrogen line measurements carried out with the FORT receiver of the meridian transit Nançay radiotelescope (NRT) in the period April 2003 -- March 2005. This observational programme is part of a larger project aiming at collecting an exhaustive and magnitude-complete HI extragalactic catalogue for Tully-Fisher applications (the so-called KLUN project, for Kinematics of the Local Universe studies, end in 2008). The whole on-line HI archive of the NRT contains today reduced HI-profiles for ~4500 spiral galaxies of declination delta > -40° (http://kl…
We use spiral galaxy evolution models to argue that there are substantial variations in stellar mass-to-light ratio (M/L) within and among galaxies. Our models show a strong correlation between stellar M/L and galaxy color. We compare the colors and maximum-disk M/L values of a sample of galaxies to the model color-M/L relation, finding that a Salpeter IMF is too massive but that an IMF with fewer low mass stars fits the observations well. Applying our color-M/L relation to the Tully-Fisher (TF) relation, we find a stellar mass TF-relation that is independent of originating passband. Adding th…
This study assesses the utility of applying the Tully-Fisher (TF) relation using photometric data from the 2MASS project. This is achieved by performing a preliminary analysis using 2MASS extended source data with the SCI sample of Giovanelli et al. (1997). Distances and peculiar velocities are measured for 11 clusters out to approx. 75/h Mpc. Statistics are found to be limited by the 47% coverage of the current 2MASS second incremental release. However, the 2MASS J, H and K-band photometry produce results in good agreement with those derived from the SCI I-band data. These results are also ge…
The Tully-Fisher relation is a correlation between the luminosity and the HI 21cm line width in spiral galaxies (LLW relation). It is used to derive galaxy distances in the interval 7 to 100 Mpc. Closer, the Cepheids, TRGB and Surface Brightness Fluctuation methods give a better accuracy. Further, the SNIa are luminous objects still available for distance measurement purposes, though with a dramatically lower density grid of measurements on the sky. Galaxies in clusters are all at the same distance from the observer. Thus the distance of the cluster derived from a large number of galaxies (N) …
Extended, soft X-ray emission from the halo of a very large disk galaxy has been detected out to r~20-40 kpc. The luminosity and surface brightness distribution is in very good agreement with predictions by recent, cosmological galaxy formation models. Predictions of Ly-alpha emission, associated with ``cold'' accretion of filamentary gas onto galaxies, are presented. In particular these predictions are compared to the properties of a recently detected Ly-alpha ``blob'', which shows no obvious continuum counter-part in any of 12 broad-bands, from X-rays (Chandra) to infrared (Spitzer). Finally…
Using moderate-resolution Keck spectra, we have examined the velocity profiles of 15 members of cluster Cl0024+1654 at z=0.4. WFPC2 images of the cluster members have been used to determine structural parameters, including disk sizes, orientations, and inclinations. We compare two methods of optical rotation curve analysis for kinematic measurements. Both methods take seeing, slit size and orientation, and instrumental effects into account and yield similar rotation velocity measurements. Four of the galaxies in our sample exhibit unusual kinematic signatures, such as non-circular motions. Our…
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 Iab <=22.5 and W_0(OII)>=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 ha…
We first discuss why the uncomfortable fine-tuning of the parameters of the Lambda-CDM cosmological model provides continuing, strong motivation to investigate Hubble's Constant. Then we review evidence from the HST Key Project that there is a significant scale error between raw Cepheid and Tully-Fisher distances. An analysis of mainly HST Distance Scale Key Project data shows a correlation between host galaxy metallicity and the rms scatter around the Cepheid P-L relation, which may support a recent suggestion that the P-L metallicity dependence is stronger than expected. If Cepheids do have …
Using a combination of Keck spectroscopy and near-infrared imaging, we investigate the K-band and stellar mass Tully-Fisher relation for 101 disk galaxies at 0.2 < z < 1.2, with the goal of placing the first observational constraints on the assembly history of halo and stellar mass. Our main result is a lack of evolution in either the K-band or stellar mass Tully-Fisher relation from z = 0 - 1.2. Furthermore, although our sample is not statistically complete, we consider it suitable for an initial investigation of how the fraction of total mass that has condensed into stars is distributed with…
We study the evolution of the [O/Fe]-[Fe/H] relation and the dependence of the iron abundance on distance from the galactic plane z in a one-zone model for a disk galaxy, starting from the beginning of star formation (Wiebe98). We obtain good agreement with the observational data, including, for the first time, agreement for the [Fe/H]-z relation out to heights of 16 kpc. We also study the influence of the presence of dark matter in the galaxies on the star-formation rate. Comparison of the observed luminosity of the Galaxy with the model prediction places constraints on the fractional mass of…
We use kinematic measurements of a large sample of galaxies from the Team Keck Redshift Survey in the GOODS-N field to measure evolution in the optical and near-IR Tully-Fisher relations to z = 1.2. We construct Tully-Fisher relations with integrated line-of-sight velocity widths of ~ 1000 galaxies in B and ~ 670 in J-band; these relations have large scatter, and we derive a maximum-likelihood least squares method for fitting in the presence of scatter. The B-band Tully-Fisher relations, from z=0.4 to z=1.2, show evolution of ~ 1.0-1.5 mag internal to our sample without requiring calibration t…
The evolution of the line width - luminosity relation for spiral galaxies, the Tully-Fisher relation, strongly constrains galaxy formation and evolution models. At this moment, the kinematics of z>1 spiral galaxies can only be measured using rest frame optical emission lines associated with star formation, such as Halpha and [OIII]5007/4959 and [OII]3727. This method has intrinsic difficulties and uncertainties. Moreover, observations of these lines are challenging for present day telescopes and techniques. Here, we present an overview of the intrinsic and observational challenges and some way…
We describe the first results of a programme to obtain rotation curves of z~1 disc galaxies in the near-infrared using the Ha emission line in order to study the Tully-Fisher relation. To put any observed evolution into perspective and to investigate any possible selection biases, we constructed a control sample of low redshift galaxies that had rotation velocities and images available for measuring their dynamical, photometric, and morphological properties. Compared to local objects with isophotal sizes similar to the high redshift targets, we find that our sample of galaxies with spatially r…
We have obtained I band Tully-Fisher (TF) measurements for 522 late-type galaxies in the fields of 52 rich Abell clusters distributed throughout the sky between 50 and 200\h Mpc. Here we estimate corrections to the data for various forms of observational bias, most notably Malmquist and cluster population incompleteness bias. The bias-corrected data are applied to the construction of an I band TF template, resulting in a relation with a dispersion of 0.38 magnitudes and a kinematical zero-point accurate to 0.02 magnitudes. This represents the most accurate TF template relation currently availa…
We discuss the origin of the Tully-Fisher (TF) relation using the $N$-body/SPH method, which includes cooling, star formation and stellar feedback of energy, mass and metals. We consider initially rotating overdense spheres, and trace formation processes of disk galaxies from $z=25$ to $z=0$ in the Cold Dark Matter (CDM) cosmology. To clarify the origin of the TF relation, we simulate formation of 14 galaxies with different masses and spin parameters, and compute observable values, such as the total magnitude and the line-width. We find that the simulated galaxies reproduce the slope and scatt…
The frequency shift of spectral lines is most often explained by the Doppler Effect in terms of relative motion, whereas the Doppler broadening of a particular line mainly depends on the absolute temperature. The Wolf effect on the other hand deals with the correlation induced spectral change and explains both the broadening and shift of the spectral lines. In this framework a relation between the width of the spectral line is related to the redshift z for the line and hence with the distance. For smaller values of z a relation similar to the Tully-Fisher relation can be obtained and for large…
Recent observations of distant disk galaxies show that there is little to no evolution in the relation between maximum rotation speed and stellar mass at z < 1.2. There is however a significant scatter between these two quantities whose origin is uncertain. We show in this paper that this scatter is at least partially the result of galaxy merging, revealing that disk galaxy growth at z < 1 is fundamentally hierarchical. We carry this out by calculating CAS (concentration, asymmetry, clumpiness) structural parameters using archival Hubble Space Telescope imaging of 91 high-redshift disk galaxie…
The Baryonic Tully-Fisher relation (BTF) can be substantially improved when considering that the galactic baryonic mass is likely to consist not only from the detected baryons, stars and gas, but also from a dark baryonic component proportional to the HI gas. The BTF relation is optimally improved when the HI mass is multiplied by a factor of about 3, but larger factors up to 11-16 still improve the fit over the original one using only the detected baryons. The strength of this improved relation is quantified with up-to-date statistical tests such as the Akaike Information Criterion or the Bay…
We investigate the influence of the star formation rate on the Tully-Fisher relation. We find that a simple model which combines the empirically-determined star-formation rate with the expected properties of galaxy halos provides a remarkably good fit to the absolute magnitude-rotation speed correlation. We find that the power-law nature, its slope, normalisation and scatter, are all readily accounted for if the Universe has a low density parameter, with or without a cosmological constant and disks are assembled at $z \sim 1 - 1.5$. Moreover, this agreement is found simultaneously in 4 waveban…
