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The SAMI Galaxy Survey: the low-redshift stellar mass Tully–Fisher relation

Bloom, J. V. and Croom, S. M. and Bryant, J. J. and Callingham, J. R. and Schaefer, A. L. and Cortese, L. and Hopkins, A. M. and D'Eugenio, F. and Scott, N. and Glazebrook, K. and Tonini, C. and McElroy, R. E. and Clark, H. A. and Catinella, B. and Allen, J. T. and Bland-Hawthorn, J. and Goodwin, M. and Green, A. W. and Konstantopoulos, I. S. and Lawrence, J. and Lorente, N. and Medling, A. M. and Owers, M. S. and Richards, S. N. and Sharp, R. (2017) The SAMI Galaxy Survey: the low-redshift stellar mass Tully–Fisher relation. Monthly Notices of the Royal Astronomical Society, 472 (2). pp. 1809-1824. ISSN 0035-8711. https://resolver.caltech.edu/CaltechAUTHORS:20171102-123817459

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Abstract

We investigate the Tully–Fisher relation (TFR) for a morphologically and kinematically diverse sample of galaxies from the Sydney-AAO Multi-object Integral field spectrograph (SAMI) Galaxy Survey using two-dimensional spatially resolved H α velocity maps and find a well-defined relation across the stellar mass range of 8.0 < log (M*/M⊙) < 11.5. We use an adaptation of kinemetry to parametrize the kinematic H α asymmetry of all galaxies in the sample, and find a correlation between scatter (i.e. residuals off the TFR) and asymmetry. This effect is pronounced at low stellar mass, corresponding to the inverse relationship between stellar mass and kinematic asymmetry found in previous work. For galaxies with log (M*/M⊙) < 9.5, 25 ± 3 per cent are scattered below the root mean square (RMS) of the TFR, whereas for galaxies with log (M*/M⊙) > 9.5 the fraction is 10 ± 1 per cent. We use ‘simulated slits’ to directly compare our results with those from long slit spectroscopy and find that aligning slits with the photometric, rather than the kinematic, position angle, increases global scatter below the TFR. Further, kinematic asymmetry is correlated with misalignment between the photometric and kinematic position angles. This work demonstrates the value of 2D spatially resolved kinematics for accurate TFR studies; integral field spectroscopy reduces the underestimation of rotation velocity that can occur from slit positioning off the kinematic axis.


Item Type:Article
Related URLs:
URLURL TypeDescription
https://doi.org/10.1093/mnras/stx1701DOIArticle
ORCID:
AuthorORCID
Croom, S. M.0000-0003-2880-9197
Bryant, J. J.0000-0003-1627-9301
Cortese, L.0000-0002-7422-9823
Hopkins, A. M.0000-0002-6097-2747
Scott, N.0000-0001-8495-8547
Bland-Hawthorn, J.0000-0001-7516-4016
Konstantopoulos, I. S.0000-0003-2177-0146
Lorente, N.0000-0003-0450-4807
Medling, A. M.0000-0001-7421-2944
Owers, M. S.0000-0002-2879-1663
Richards, S. N.0000-0002-5368-0068
Additional Information:© 2017 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society. Accepted 2017 July 4. Received 2017 July 4; in original form 2017 May 5. Published: 19 July 2017. The SAMI Galaxy Survey is based on observations made at the Anglo-Australian Telescope. The Sydney-AAO Multi-object Integral field spectrograph (SAMI) was developed jointly by the University of Sydney and the Australian Astronomical Observatory. The SAMI input catalogue is based on data taken from the Sloan Digital Sky Survey, the GAMA Survey and the VST ATLAS Survey. The SAMI Galaxy Survey is funded by the Australian Research Council Centre of Excellence for All-sky Astrophysics (CAASTRO), through project number CE110001020, and other participating institutions. The SAMI Galaxy Survey website is http://sami-survey.org/. GAMA is a joint European-Australasian project based around a spectroscopic campaign using the Anglo-Australian Telescope. The GAMA input catalogue is based on data taken from the Sloan Digital Sky Survey and the UKIRT Infrared Deep Sky Survey. Complementary imaging of the GAMA regions is being obtained by a number of independent survey programmes including GALEX MIS, VST KiDS, VISTA VIKING, WISE, Herschel-ATLAS, GMRT ASKAP providing UV to radio coverage. GAMA is funded by the STFC (UK), the ARC (Australia), the AAO and the participating institutions. The GAMA website is http://www.gama-survey.org/. Support for AMM is provided by NASA through Hubble Fellowship grant # HST-HF2-51377 awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS5-26555. SMC acknowledges the support of an Australian Research Council Future Fellowship (FT100100457). MSO acknowledges the funding support from the Australian Research Council through a Future Fellowship (FT140100255). We thank the referee for their helpful and insightful comments, which clarified and improved the paper.
Funders:
Funding AgencyGrant Number
Australian Research CouncilCE110001020
NASA Hubble FellowshipHST-HF2-51377
NASANAS5-26555
Australian Research CouncilFT100100457
Australian Research CouncilFT140100255
Subject Keywords:techniques: imaging spectroscopy – galaxies: evolution – galaxies: kinematics and dynamics – galaxies: structure
Issue or Number:2
Record Number:CaltechAUTHORS:20171102-123817459
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20171102-123817459
Official Citation:J. V. Bloom, S. M. Croom, J. J. Bryant, J. R. Callingham, A. L. Schaefer, L. Cortese, A. M. Hopkins, F. D'Eugenio, N. Scott, K. Glazebrook, C. Tonini, R. E. McElroy, H. A. Clark, B. Catinella, J. T. Allen, J. Bland-Hawthorn, M. Goodwin, A. W. Green, I. S. Konstantopoulos, J. Lawrence, N. Lorente, A. M. Medling, M. S. Owers, S. N. Richards, R. Sharp; The SAMI Galaxy Survey: the low-redshift stellar mass Tully–Fisher relation, Monthly Notices of the Royal Astronomical Society, Volume 472, Issue 2, 1 December 2017, Pages 1809–1824, https://doi.org/10.1093/mnras/stx1701
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:82897
Collection:CaltechAUTHORS
Deposited By: Tony Diaz
Deposited On:02 Nov 2017 19:56
Last Modified:09 Mar 2020 13:18

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