The I Band Tully-Fisher Relation for Cluster Galaxies: a Template Relation, its Scatter and Bias Corrections.

Abstract

Infrared I band photometry and velocity widths for galaxies in 24 clusters, with radial velocities between 1,000 and 10,000 km s −1 , are used to construct a template Tully-Fisher (TF) relation. The sources of scatter in the TF diagram are analyzed in detail; it is shown that the common practice of referring to a single figure of TF scatter is incorrect and can lead to erroneous bias corrections. Biases resulting from sample incompleteness, catalog inaccuracies, cluster size and other sources, as well as dependences of TF parameters on morphological type and local environment, are discussed and appropriate corrections are obtained. A template TF relation is constructed by combining the data from the 24 clusters, and kinematic cluster offsets from a putative reference frame which well approximates null velocity with respect to the cosmic microwave background, are obtained.

The Spectroscopy and H-band Imaging of Virgo Cluster Galaxies (SHIVir) Survey: Scaling Relations and the Stellar-to-total Mass Relation

“…for ALFALFA. Also shown are cluster and field TF fits for other non-Virgo source catalogs (Giovanelli et al 1997;Neistein et al 1999;Courteau et al 2007a;Pizagno et al 2007;Hall et al 2012). Our best TFR for VCGs (see Table 1) is shown as a solid black line.…”

“…While the TFR has been studied extensively (e.g., Courteau 1997; Giovanelli et al 1997;McGaugh et al 2000;Courteau et al 2007a;Pizagno et al 2007;Hall et al 2012;Bekeraité et al 2016;Bradford et al 2016, to list a few), differences between field and cluster environments remain illconstrained especially in the context of the Virgo cluster, where stripping effects have been well documented (e.g., Koopmann & Kenney 2004). We have compiled a subsample of 46 Virgo LTGs with resolved Hα RCs that could successfully be fitted using themultiparameter function in Equation (1).…”

“…This is largely due to our smaller sample size and greater distance errors (as the 3D structure of the Virgo cluster is poorly determined). Typically, the TFR scatter found for samples containing a few hundred galaxies is on the order of 0.2 to 0.5 mag (Courteau 1997;Giovanelli et al 1997). Since our LTG sample is relatively small, the fit uncertainty should be proportionally larger.…”

“…Superimposed on the data in Figure 6 are additional TFRs based on i-band photometry for cluster (Giovanelli et al 1997;Neistein et al 1999;Hall et al 2012) and field environments (Courteau et al 2007a;Pizagno et al 2007). Despite ram pressure stripping and tidal interactions in cluster environments, which affect star formation rates, and thus galaxy luminosities, more effectively than in the field (Koopmann & Kenney 2004), and while Virgo RCs are truncated relative to field analogs, the VCG data nicely match other cluster and field TF distributions.…”

The Effect of Filaments and Tendrils on the H i Content of Galaxies

“…The channel range of the galaxy is estimated using the Tully-Fisher relation and the SDSS i-band magnitude following Giovanelli et al (1997), adopting γ = 1.0 in the internal extinction correction ∆m = −γ log(a/b) (their equation 8), which is appropriate for all but the brightest galaxies and overcorrects for fainter galaxies (see Figure 7c of Giovanelli et al 1995); this ensures the rms is measured outside any possible galaxy signal. We fit the baseline with a first-order polynomial and calculate the rms about this fit, using the Arecibo IDL program robfit poly.pro by Phil Perrilat.…”