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Title: The calibration of the WISE W1 and W2 Tully-Fisher relation

Abstract

In order to explore local large-scale structures and velocity fields, accurate galaxy distance measures are needed. We now extend the well-tested recipe for calibrating the correlation between galaxy rotation rates and luminosities—capable of providing such distance measures—to the all-sky, space-based imaging data from the Wide-field Infrared Survey Explorer (WISE) W1 (3.4 μm) and W2 (4.6 μm) filters. We find a correlation of line width to absolute magnitude (known as the Tully-Fisher relation, TFR) of M{sub W1}{sup b,i,k,a}=−20.35−9.56(log W{sub mx}{sup i}−2.5) (0.54 mag rms) and M{sub W2}{sup b,i,k,a}=−19.76−9.74(log W{sub mx}{sup i}−2.5) (0.56 mag rms) from 310 galaxies in 13 clusters. We update the I-band TFR using a sample 9% larger than in Tully and Courtois. We derive M{sub I}{sup b,i,k}=−21.34−8.95(log W{sub mx}{sup i}−2.5) (0.46 mag rms). The WISE TFRs show evidence of curvature. Quadratic fits give M{sub W1}{sup b,i,k,a}=−20.48−8.36(log W{sub mx}{sup i}−2.5)+3.60(log W{sub mx}{sup i}−2.5){sup 2} (0.52 mag rms) and M{sub W2}{sup b,i,k,a}=−19.91−8.40(log W{sub mx}{sup i}−2.5)+4.32(log W{sub mx}{sup i}−2.5){sup 2} (0.55 mag rms). We apply an I-band –WISE color correction to lower the scatter and derive M{sub C{sub W{sub 1}}}=−20.22−9.12(log W{sub mx}{sup i}−2.5) and M{sub C{sub W{sub 2}}}=−19.63−9.11(log W{sub mx}{sup i}−2.5) (both 0.46 mag rms). Using our three independent TFRs (W1 curved, W2 curved, and I band), we calibrate themore » UNION2 Type Ia supernova sample distance scale and derive H {sub 0} = 74.4 ± 1.4(stat) ± 2.4(sys) km s{sup –1} Mpc{sup –1} with 4% total error.« less

Authors:
 [1]; ;  [2];  [3]; ;  [4];  [5];  [6]
  1. California Institute of Technology, 1200 East California Boulevard, MC 278-17, Pasadena, CA 91125 (United States)
  2. The Observatories of the Carnegie Institute of Washington, 813 Santa Barbara Street, Pasadena, CA 91101 (United States)
  3. Institute for Astronomy, University of Hawaii, 2680 Woodlawn Drive, Honolulu, HI 96822 (United States)
  4. Institut de Physique Nucleaire, Université Claude Bernard Lyon I, F-69100 Lyon (France)
  5. University of Cape Town, Private Bag X3, Rondebosch 7701, Republic of South Africa (South Africa)
  6. Image Processing and Analysis Center (IPAC), California Institute of Technology, 1200 East California Boulevard, MC 100-22, Pasadena, CA 91125 (United States)
Publication Date:
OSTI Identifier:
22365090
Resource Type:
Journal Article
Journal Name:
Astrophysical Journal
Additional Journal Information:
Journal Volume: 792; Journal Issue: 2; Other Information: Country of input: International Atomic Energy Agency (IAEA); Journal ID: ISSN 0004-637X
Country of Publication:
United States
Language:
English
Subject:
79 ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; CALIBRATION; COLOR; CORRECTIONS; CORRELATIONS; DISTANCE; ERRORS; GALAXIES; GALAXY CLUSTERS; INFRARED SURVEYS; LINE WIDTHS; LUMINOSITY; PHOTOMETRY; RED SHIFT; ROTATION; SPACE

Citation Formats

Neill, J. D., Seibert, Mark, Scowcroft, Victoria, Tully, R. Brent, Courtois, Hélène, Sorce, Jenny G., Jarrett, T. H., and Masci, Frank J. The calibration of the WISE W1 and W2 Tully-Fisher relation. United States: N. p., 2014. Web. doi:10.1088/0004-637X/792/2/129.
Neill, J. D., Seibert, Mark, Scowcroft, Victoria, Tully, R. Brent, Courtois, Hélène, Sorce, Jenny G., Jarrett, T. H., & Masci, Frank J. The calibration of the WISE W1 and W2 Tully-Fisher relation. United States. doi:10.1088/0004-637X/792/2/129.
Neill, J. D., Seibert, Mark, Scowcroft, Victoria, Tully, R. Brent, Courtois, Hélène, Sorce, Jenny G., Jarrett, T. H., and Masci, Frank J. Wed . "The calibration of the WISE W1 and W2 Tully-Fisher relation". United States. doi:10.1088/0004-637X/792/2/129.
@article{osti_22365090,
title = {The calibration of the WISE W1 and W2 Tully-Fisher relation},
author = {Neill, J. D. and Seibert, Mark and Scowcroft, Victoria and Tully, R. Brent and Courtois, Hélène and Sorce, Jenny G. and Jarrett, T. H. and Masci, Frank J.},
abstractNote = {In order to explore local large-scale structures and velocity fields, accurate galaxy distance measures are needed. We now extend the well-tested recipe for calibrating the correlation between galaxy rotation rates and luminosities—capable of providing such distance measures—to the all-sky, space-based imaging data from the Wide-field Infrared Survey Explorer (WISE) W1 (3.4 μm) and W2 (4.6 μm) filters. We find a correlation of line width to absolute magnitude (known as the Tully-Fisher relation, TFR) of M{sub W1}{sup b,i,k,a}=−20.35−9.56(log W{sub mx}{sup i}−2.5) (0.54 mag rms) and M{sub W2}{sup b,i,k,a}=−19.76−9.74(log W{sub mx}{sup i}−2.5) (0.56 mag rms) from 310 galaxies in 13 clusters. We update the I-band TFR using a sample 9% larger than in Tully and Courtois. We derive M{sub I}{sup b,i,k}=−21.34−8.95(log W{sub mx}{sup i}−2.5) (0.46 mag rms). The WISE TFRs show evidence of curvature. Quadratic fits give M{sub W1}{sup b,i,k,a}=−20.48−8.36(log W{sub mx}{sup i}−2.5)+3.60(log W{sub mx}{sup i}−2.5){sup 2} (0.52 mag rms) and M{sub W2}{sup b,i,k,a}=−19.91−8.40(log W{sub mx}{sup i}−2.5)+4.32(log W{sub mx}{sup i}−2.5){sup 2} (0.55 mag rms). We apply an I-band –WISE color correction to lower the scatter and derive M{sub C{sub W{sub 1}}}=−20.22−9.12(log W{sub mx}{sup i}−2.5) and M{sub C{sub W{sub 2}}}=−19.63−9.11(log W{sub mx}{sup i}−2.5) (both 0.46 mag rms). Using our three independent TFRs (W1 curved, W2 curved, and I band), we calibrate the UNION2 Type Ia supernova sample distance scale and derive H {sub 0} = 74.4 ± 1.4(stat) ± 2.4(sys) km s{sup –1} Mpc{sup –1} with 4% total error.},
doi = {10.1088/0004-637X/792/2/129},
journal = {Astrophysical Journal},
issn = {0004-637X},
number = 2,
volume = 792,
place = {United States},
year = {2014},
month = {9}
}