THE SPITZER SURVEY of STELLAR STRUCTURE in GALAXIES (S4G): PRECISE STELLAR MASS DISTRIBUTIONS from AUTOMATED DUST CORRECTION at 3.6 μm

Miguel Querejeta, Sharon E. Meidt, Eva Schinnerer, Mauricio Cisternas, Juan Carlos Muñoz-Mateos, Kartik Sheth, Johan Knapen, Glenn Van De Ven, Mark A. Norris, Reynier Peletier, Eija Laurikainen, Heikki Salo, Benne W. Holwerda, E. Athanassoula, Albert Bosma, Brent Groves, Luis C. Ho, Dimitri A. Gadotti, Dennis F Zaritsky, Michael ReganJoannah Hinz, Armando Gil De Paz, Karin Menendez-Delmestre, Mark Seibert, Trisha Mizusawa, Taehyun Kim, Santiago Erroz-Ferrer, Jarkko Laine, Sébastien Comerón

Research output: Contribution to journalArticle

79 Citations (Scopus)

Abstract

The mid-infrared is an optimal window to trace stellar mass in nearby galaxies and the 3.6 mm IRAC band has been exploited to this effect, but such mass estimates can be biased by dust emission. We present our pipeline to reveal the old stellar flux at 3.6 μm and obtain stellar mass maps for more than 1600 galaxies available from the Spitzer Survey of Stellar Structure in Galaxies (S4G). This survey consists of images in two infrared bands (3.6 and 4.5 μm), and we use the Independent Component Analysis (ICA) method presented in Meidt et al. to separate the dominant light from old stars and the dust emission that can significantly contribute to the observed 3.6 mm flux. We exclude from our ICA analysis galaxies with low signal-to-noise ratio (S/N <10) and those with original [3.6][4.5] colors compatible with an old stellar population, indicative of little dust emission (mostly early Hubble types, which can directly provide good mass maps). For the remaining 1251 galaxies to which ICA was successfully applied, we find that as much as 10%30% of the total light at 3.6 μm typically originates from dust, and locally it can reach even higher values. This contamination fraction shows a correlation with specific star formation rates, confirming that the dust emission that we detect is related to star formation. Additionally, we have used our large sample of mass estimates to calibrate a relationship of effective mass-to-light ratio (M/L) as a function of observed [3.6][4.5] color: log(M/L) = -0.339(±0.057) × ([3.6]-[4.5]) - 0.336(±0.002). Our final pipeline products have been made public through IRSA, providing the astronomical community with an unprecedentedly large set of stellar mass maps ready to use for scientific applications.

Original languageEnglish (US)
Article number5
JournalAstrophysical Journal, Supplement Series
Volume219
Issue number1
DOIs
StatePublished - Jul 20 2015
Externally publishedYes

Fingerprint

stellar mass
mass distribution
dust
galaxies
stellar structure
color
mass to light ratios
estimates
star formation rate
star formation
contamination
signal to noise ratios
distribution
signal-to-noise ratio
stars
products
analysis

Keywords

  • galaxies: evolution
  • galaxies: formation
  • galaxies: photometry
  • galaxies: structure

ASJC Scopus subject areas

  • Space and Planetary Science
  • Astronomy and Astrophysics

Cite this

THE SPITZER SURVEY of STELLAR STRUCTURE in GALAXIES (S4G) : PRECISE STELLAR MASS DISTRIBUTIONS from AUTOMATED DUST CORRECTION at 3.6 μm. / Querejeta, Miguel; Meidt, Sharon E.; Schinnerer, Eva; Cisternas, Mauricio; Muñoz-Mateos, Juan Carlos; Sheth, Kartik; Knapen, Johan; Ven, Glenn Van De; Norris, Mark A.; Peletier, Reynier; Laurikainen, Eija; Salo, Heikki; Holwerda, Benne W.; Athanassoula, E.; Bosma, Albert; Groves, Brent; Ho, Luis C.; Gadotti, Dimitri A.; Zaritsky, Dennis F; Regan, Michael; Hinz, Joannah; Paz, Armando Gil De; Menendez-Delmestre, Karin; Seibert, Mark; Mizusawa, Trisha; Kim, Taehyun; Erroz-Ferrer, Santiago; Laine, Jarkko; Comerón, Sébastien.

In: Astrophysical Journal, Supplement Series, Vol. 219, No. 1, 5, 20.07.2015.

Research output: Contribution to journalArticle

Querejeta, M, Meidt, SE, Schinnerer, E, Cisternas, M, Muñoz-Mateos, JC, Sheth, K, Knapen, J, Ven, GVD, Norris, MA, Peletier, R, Laurikainen, E, Salo, H, Holwerda, BW, Athanassoula, E, Bosma, A, Groves, B, Ho, LC, Gadotti, DA, Zaritsky, DF, Regan, M, Hinz, J, Paz, AGD, Menendez-Delmestre, K, Seibert, M, Mizusawa, T, Kim, T, Erroz-Ferrer, S, Laine, J & Comerón, S 2015, 'THE SPITZER SURVEY of STELLAR STRUCTURE in GALAXIES (S4G): PRECISE STELLAR MASS DISTRIBUTIONS from AUTOMATED DUST CORRECTION at 3.6 μm', Astrophysical Journal, Supplement Series, vol. 219, no. 1, 5. https://doi.org/10.1088/0067-0049/219/1/5
Querejeta, Miguel ; Meidt, Sharon E. ; Schinnerer, Eva ; Cisternas, Mauricio ; Muñoz-Mateos, Juan Carlos ; Sheth, Kartik ; Knapen, Johan ; Ven, Glenn Van De ; Norris, Mark A. ; Peletier, Reynier ; Laurikainen, Eija ; Salo, Heikki ; Holwerda, Benne W. ; Athanassoula, E. ; Bosma, Albert ; Groves, Brent ; Ho, Luis C. ; Gadotti, Dimitri A. ; Zaritsky, Dennis F ; Regan, Michael ; Hinz, Joannah ; Paz, Armando Gil De ; Menendez-Delmestre, Karin ; Seibert, Mark ; Mizusawa, Trisha ; Kim, Taehyun ; Erroz-Ferrer, Santiago ; Laine, Jarkko ; Comerón, Sébastien. / THE SPITZER SURVEY of STELLAR STRUCTURE in GALAXIES (S4G) : PRECISE STELLAR MASS DISTRIBUTIONS from AUTOMATED DUST CORRECTION at 3.6 μm. In: Astrophysical Journal, Supplement Series. 2015 ; Vol. 219, No. 1.
@article{e2124e7ca4ff4fe6a4175fcf427fa9a9,
title = "THE SPITZER SURVEY of STELLAR STRUCTURE in GALAXIES (S4G): PRECISE STELLAR MASS DISTRIBUTIONS from AUTOMATED DUST CORRECTION at 3.6 μm",
abstract = "The mid-infrared is an optimal window to trace stellar mass in nearby galaxies and the 3.6 mm IRAC band has been exploited to this effect, but such mass estimates can be biased by dust emission. We present our pipeline to reveal the old stellar flux at 3.6 μm and obtain stellar mass maps for more than 1600 galaxies available from the Spitzer Survey of Stellar Structure in Galaxies (S4G). This survey consists of images in two infrared bands (3.6 and 4.5 μm), and we use the Independent Component Analysis (ICA) method presented in Meidt et al. to separate the dominant light from old stars and the dust emission that can significantly contribute to the observed 3.6 mm flux. We exclude from our ICA analysis galaxies with low signal-to-noise ratio (S/N <10) and those with original [3.6][4.5] colors compatible with an old stellar population, indicative of little dust emission (mostly early Hubble types, which can directly provide good mass maps). For the remaining 1251 galaxies to which ICA was successfully applied, we find that as much as 10{\%}30{\%} of the total light at 3.6 μm typically originates from dust, and locally it can reach even higher values. This contamination fraction shows a correlation with specific star formation rates, confirming that the dust emission that we detect is related to star formation. Additionally, we have used our large sample of mass estimates to calibrate a relationship of effective mass-to-light ratio (M/L) as a function of observed [3.6][4.5] color: log(M/L) = -0.339(±0.057) × ([3.6]-[4.5]) - 0.336(±0.002). Our final pipeline products have been made public through IRSA, providing the astronomical community with an unprecedentedly large set of stellar mass maps ready to use for scientific applications.",
keywords = "galaxies: evolution, galaxies: formation, galaxies: photometry, galaxies: structure",
author = "Miguel Querejeta and Meidt, {Sharon E.} and Eva Schinnerer and Mauricio Cisternas and Mu{\~n}oz-Mateos, {Juan Carlos} and Kartik Sheth and Johan Knapen and Ven, {Glenn Van De} and Norris, {Mark A.} and Reynier Peletier and Eija Laurikainen and Heikki Salo and Holwerda, {Benne W.} and E. Athanassoula and Albert Bosma and Brent Groves and Ho, {Luis C.} and Gadotti, {Dimitri A.} and Zaritsky, {Dennis F} and Michael Regan and Joannah Hinz and Paz, {Armando Gil De} and Karin Menendez-Delmestre and Mark Seibert and Trisha Mizusawa and Taehyun Kim and Santiago Erroz-Ferrer and Jarkko Laine and S{\'e}bastien Comer{\'o}n",
year = "2015",
month = "7",
day = "20",
doi = "10.1088/0067-0049/219/1/5",
language = "English (US)",
volume = "219",
journal = "Astrophysical Journal, Supplement Series",
issn = "0067-0049",
publisher = "IOP Publishing Ltd.",
number = "1",

}

TY - JOUR

T1 - THE SPITZER SURVEY of STELLAR STRUCTURE in GALAXIES (S4G)

T2 - PRECISE STELLAR MASS DISTRIBUTIONS from AUTOMATED DUST CORRECTION at 3.6 μm

AU - Querejeta, Miguel

AU - Meidt, Sharon E.

AU - Schinnerer, Eva

AU - Cisternas, Mauricio

AU - Muñoz-Mateos, Juan Carlos

AU - Sheth, Kartik

AU - Knapen, Johan

AU - Ven, Glenn Van De

AU - Norris, Mark A.

AU - Peletier, Reynier

AU - Laurikainen, Eija

AU - Salo, Heikki

AU - Holwerda, Benne W.

AU - Athanassoula, E.

AU - Bosma, Albert

AU - Groves, Brent

AU - Ho, Luis C.

AU - Gadotti, Dimitri A.

AU - Zaritsky, Dennis F

AU - Regan, Michael

AU - Hinz, Joannah

AU - Paz, Armando Gil De

AU - Menendez-Delmestre, Karin

AU - Seibert, Mark

AU - Mizusawa, Trisha

AU - Kim, Taehyun

AU - Erroz-Ferrer, Santiago

AU - Laine, Jarkko

AU - Comerón, Sébastien

PY - 2015/7/20

Y1 - 2015/7/20

N2 - The mid-infrared is an optimal window to trace stellar mass in nearby galaxies and the 3.6 mm IRAC band has been exploited to this effect, but such mass estimates can be biased by dust emission. We present our pipeline to reveal the old stellar flux at 3.6 μm and obtain stellar mass maps for more than 1600 galaxies available from the Spitzer Survey of Stellar Structure in Galaxies (S4G). This survey consists of images in two infrared bands (3.6 and 4.5 μm), and we use the Independent Component Analysis (ICA) method presented in Meidt et al. to separate the dominant light from old stars and the dust emission that can significantly contribute to the observed 3.6 mm flux. We exclude from our ICA analysis galaxies with low signal-to-noise ratio (S/N <10) and those with original [3.6][4.5] colors compatible with an old stellar population, indicative of little dust emission (mostly early Hubble types, which can directly provide good mass maps). For the remaining 1251 galaxies to which ICA was successfully applied, we find that as much as 10%30% of the total light at 3.6 μm typically originates from dust, and locally it can reach even higher values. This contamination fraction shows a correlation with specific star formation rates, confirming that the dust emission that we detect is related to star formation. Additionally, we have used our large sample of mass estimates to calibrate a relationship of effective mass-to-light ratio (M/L) as a function of observed [3.6][4.5] color: log(M/L) = -0.339(±0.057) × ([3.6]-[4.5]) - 0.336(±0.002). Our final pipeline products have been made public through IRSA, providing the astronomical community with an unprecedentedly large set of stellar mass maps ready to use for scientific applications.

AB - The mid-infrared is an optimal window to trace stellar mass in nearby galaxies and the 3.6 mm IRAC band has been exploited to this effect, but such mass estimates can be biased by dust emission. We present our pipeline to reveal the old stellar flux at 3.6 μm and obtain stellar mass maps for more than 1600 galaxies available from the Spitzer Survey of Stellar Structure in Galaxies (S4G). This survey consists of images in two infrared bands (3.6 and 4.5 μm), and we use the Independent Component Analysis (ICA) method presented in Meidt et al. to separate the dominant light from old stars and the dust emission that can significantly contribute to the observed 3.6 mm flux. We exclude from our ICA analysis galaxies with low signal-to-noise ratio (S/N <10) and those with original [3.6][4.5] colors compatible with an old stellar population, indicative of little dust emission (mostly early Hubble types, which can directly provide good mass maps). For the remaining 1251 galaxies to which ICA was successfully applied, we find that as much as 10%30% of the total light at 3.6 μm typically originates from dust, and locally it can reach even higher values. This contamination fraction shows a correlation with specific star formation rates, confirming that the dust emission that we detect is related to star formation. Additionally, we have used our large sample of mass estimates to calibrate a relationship of effective mass-to-light ratio (M/L) as a function of observed [3.6][4.5] color: log(M/L) = -0.339(±0.057) × ([3.6]-[4.5]) - 0.336(±0.002). Our final pipeline products have been made public through IRSA, providing the astronomical community with an unprecedentedly large set of stellar mass maps ready to use for scientific applications.

KW - galaxies: evolution

KW - galaxies: formation

KW - galaxies: photometry

KW - galaxies: structure

UR - http://www.scopus.com/inward/record.url?scp=84938083671&partnerID=8YFLogxK

UR - http://www.scopus.com/inward/citedby.url?scp=84938083671&partnerID=8YFLogxK

U2 - 10.1088/0067-0049/219/1/5

DO - 10.1088/0067-0049/219/1/5

M3 - Article

AN - SCOPUS:84938083671

VL - 219

JO - Astrophysical Journal, Supplement Series

JF - Astrophysical Journal, Supplement Series

SN - 0067-0049

IS - 1

M1 - 5

ER -