# 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 »

- Authors:

- California Institute of Technology, 1200 East California Boulevard, MC 278-17, Pasadena, CA 91125 (United States)
- The Observatories of the Carnegie Institute of Washington, 813 Santa Barbara Street, Pasadena, CA 91101 (United States)
- Institute for Astronomy, University of Hawaii, 2680 Woodlawn Drive, Honolulu, HI 96822 (United States)
- Institut de Physique Nucleaire, Université Claude Bernard Lyon I, F-69100 Lyon (France)
- University of Cape Town, Private Bag X3, Rondebosch 7701, Republic of South Africa (South Africa)
- 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}

}