St Andrews Research Repository

St Andrews University Home
View Item 
  •   St Andrews Research Repository
  • University of St Andrews Research
  • University of St Andrews Research
  • University of St Andrews Research
  • View Item
  •   St Andrews Research Repository
  • University of St Andrews Research
  • University of St Andrews Research
  • University of St Andrews Research
  • View Item
  •   St Andrews Research Repository
  • University of St Andrews Research
  • University of St Andrews Research
  • University of St Andrews Research
  • View Item
  • Login
JavaScript is disabled for your browser. Some features of this site may not work without it.

The H I Tully-Fisher telation of early-type galaxies

Thumbnail
View/Open
Weijmans_2015_A_A_HITully_Fisher.pdf (504.7Kb)
Date
09/2015
Author
den Heijer, Milan
Oosterloo, Tom A.
Serra, Paolo
Jozsa, Gyula I. G.
Kerp, Juergen
Morganti, Raffaella
Cappellari, Michele
Davis, Timothy A.
Duc, Pierre-Alain
Emsellem, Eric
Krajnovic, Davor
McDermid, Richard M.
Naab, Torsten
Weijmans, Anne-Marie
de Zeeuw, P. Tim
Keywords
Galaxies: kinematics and dynamics
Galaxies: elliptical and lenticular, cD
QB Astronomy
QC Physics
3rd-DAS
Metadata
Show full item record
Altmetrics Handle Statistics
Altmetrics DOI Statistics
Abstract
We study the H iK-band Tully-Fisher relation and the baryonic Tully-Fisher relation for a sample of 16 early-type galaxies, taken from the ATLAS3D sample, which all have very regular H i disks extending well beyond the optical body (≳ 5 Reff). We use the kinematics of these disks to estimate the circular velocity at large radii for these galaxies. We find that the Tully-Fisher relation for our early-type galaxies is offset by about 0.5-0.7 mag from the relation for spiral galaxies, in the sense that early-type galaxies are dimmer for a given circular velocity. The residuals with respect to the spiral Tully-Fisher relation correlate with estimates of the stellar mass-to-light ratio, suggesting that the offset between the relations is mainly driven by differences in stellar populations. We also observe a small offset between our Tully-Fisher relation with the relation derived for the ATLAS3D sample based on CO data representing the galaxies’ inner regions (≲1 Reff). This indicates that the circular velocities at large radii are systematically 10% lower than those near 0.5−1 Reff, in line with recent determinations of the shape of the mass profile of early-type galaxies. The baryonic Tully-Fisher relation of our sample is distinctly tighter than the standard one, in particular when using mass-to-light ratios based on dynamical models of the stellar kinematics. We find that the early-type galaxies fall on the spiral baryonic Tully-Fisher relation if one assumes M/LK = 0.54 M⊙/L⊙ for the stellar populations of the spirals, a value similar to that found by recent studies of the dynamics of spiral galaxies. Such a mass-to-light ratio for spiral galaxies would imply that their disks are 60-70% of maximal. Our analysis increases the range of galaxy morphologies for which the baryonic Tully-Fisher relations holds, strengthening previous claims that it is a more fundamental scaling relation than the classical Tully-Fisher relation.
Citation
den Heijer , M , Oosterloo , T A , Serra , P , Jozsa , G I G , Kerp , J , Morganti , R , Cappellari , M , Davis , T A , Duc , P-A , Emsellem , E , Krajnovic , D , McDermid , R M , Naab , T , Weijmans , A-M & de Zeeuw , P T 2015 , ' The H I Tully-Fisher telation of early-type galaxies ' , Astronomy & Astrophysics , vol. 581 , pp. A98 . https://doi.org/10.1051/0004-6361/201526879
Publication
Astronomy & Astrophysics
Status
Peer reviewed
DOI
https://doi.org/10.1051/0004-6361/201526879
ISSN
0004-6361
Type
Journal article
Rights
Copyright ESO 2015. Reproduced with permission from Astronomy & Astrophysics, © ESO. This work is made available online in accordance with the publisher’s policies. This is the final published version of the work, which was originally published at http://dx.doi.org/10.1051/0004-6361/201526879
Description
Milan den Heijer was supported for this research through a stipend from the International Max Planck Research School (IMPRS) for Astronomy and Astrophysics at the Universities of Bonn and Cologne. Jürgen Kerp and Milan den Heijer thank the Deutsche Forschungsgemeinschaft (DFG) for support on the grants KE 757/7-2 and KE 757/9-1. M.C. acknowledges support from a Royal Society University Research Fellowship. This work was supported by the rolling grants “Astrophysics at Oxford” PP/E001114/1 and ST/H002456/1 and visitors grants PPA/V/S/2002/00553, PP/E001564/1 and ST/H504862/1 from the UK Research Councils. T.A.D. acknowledges the support provided by an ESO fellowship. T.N. acknowledges support from the DFG Cluster of Excellence “Origin and Structure of the Universe”. A.W. acknowledges support of a Leverhulme Trust Early Career Fellowship. The research leading to these results has received funding from the European Community’s Seventh Framework Programme (/FP7/2007-2013/) under grant agreement No. 229517. The authors acknowledge financial support from ESO.
Collections
  • University of St Andrews Research
URL
http://adsabs.harvard.edu/abs/2015arXiv150905236D
URI
http://hdl.handle.net/10023/7514

Items in the St Andrews Research Repository are protected by copyright, with all rights reserved, unless otherwise indicated.

Advanced Search

Browse

All of RepositoryCommunities & CollectionsBy Issue DateNamesTitlesSubjectsClassificationTypeFunderThis CollectionBy Issue DateNamesTitlesSubjectsClassificationTypeFunder

My Account

Login

Open Access

To find out how you can benefit from open access to research, see our library web pages and Open Access blog. For open access help contact: openaccess@st-andrews.ac.uk.

Accessibility

Read our Accessibility statement.

How to submit research papers

The full text of research papers can be submitted to the repository via Pure, the University's research information system. For help see our guide: How to deposit in Pure.

Electronic thesis deposit

Help with deposit.

Repository help

For repository help contact: Digital-Repository@st-andrews.ac.uk.

Give Feedback

Cookie policy

This site may use cookies. Please see Terms and Conditions.

Usage statistics

COUNTER-compliant statistics on downloads from the repository are available from the IRUS-UK Service. Contact us for information.

© University of St Andrews Library

University of St Andrews is a charity registered in Scotland, No SC013532.

  • Facebook
  • Twitter