skip to main content
OSTI.GOV title logo U.S. Department of Energy
Office of Scientific and Technical Information

Title: The Tip of the red giant branch distance to the perfect spiral galaxy M74 hosting three core-collapse supernovae

Abstract

M74 (NGC 628) is a famous face-on spiral galaxy, hosting three core-collapse supernovae (SNe): SN Ic 2002ap, SN II-P 2003gd, and SN II-P 2013ej. However, its distance is not well known. We present a distance estimation for this galaxy based on the Tip of the Red Giant Branch (TRGB) method. We obtain photometry of the resolved stars in the arm-free region of M74 from F555W and F814W images in the Hubble Space Telescope archive. The color-magnitude diagram of the resolved stars shows a dominant red giant branch (RGB) as well as blue main sequence stars, red helium burning stars, and asymptotic giant branch stars. The I-band luminosity function of the RGB stars shows the TRGB to be at I {sub TRGB} = 26.13 ± 0.03 mag, and T {sub RGB} = 25.97 ± 0.03. From this, we derive the distance modulus to M74 to be 30.04 ± 0.04 (random) ± 0.12 (systematic) (corresponding to a linear distance of 10.19 ± 0.14 ± 0.56 Mpc). With this distance estimate, we calibrate the standardized candle method for SNe II-P. From the absolute magnitudes of SN 2003gd, we derive a value of the Hubble constant, H {sub 0} = 72 ± 6 (random)more » ± 7 (systematic) km s{sup –1} Mpc{sup –1}. It is similar to recent estimates based on the luminosity calibration of Type Ia supernovae.« less

Authors:
;  [1]
  1. Astronomy Program, Department of Physics and Astronomy, Seoul National University, Gwanak-gu, Seoul 151-742 (Korea, Republic of)
Publication Date:
OSTI Identifier:
22365186
Resource Type:
Journal Article
Resource Relation:
Journal Name: Astrophysical Journal; Journal Volume: 792; Journal Issue: 1; Other Information: Country of input: International Atomic Energy Agency (IAEA)
Country of Publication:
United States
Language:
English
Subject:
79 ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; ASYMPTOTIC SOLUTIONS; CALIBRATION; COLOR; DISTANCE; GALAXIES; HELIUM BURNING; LUMINOSITY; MAIN SEQUENCE STARS; PHOTOMETRY; RANDOMNESS; RED SHIFT; SPACE; TELESCOPES; TYPE I SUPERNOVAE; TYPE II SUPERNOVAE

Citation Formats

Sung Jang, In, and Gyoon Lee, Myung, E-mail: isjang@astro.snu.ac.kr, E-mail: mglee@astro.snu.ac.kr. The Tip of the red giant branch distance to the perfect spiral galaxy M74 hosting three core-collapse supernovae. United States: N. p., 2014. Web. doi:10.1088/0004-637X/792/1/52.
Sung Jang, In, & Gyoon Lee, Myung, E-mail: isjang@astro.snu.ac.kr, E-mail: mglee@astro.snu.ac.kr. The Tip of the red giant branch distance to the perfect spiral galaxy M74 hosting three core-collapse supernovae. United States. doi:10.1088/0004-637X/792/1/52.
Sung Jang, In, and Gyoon Lee, Myung, E-mail: isjang@astro.snu.ac.kr, E-mail: mglee@astro.snu.ac.kr. Mon . "The Tip of the red giant branch distance to the perfect spiral galaxy M74 hosting three core-collapse supernovae". United States. doi:10.1088/0004-637X/792/1/52.
@article{osti_22365186,
title = {The Tip of the red giant branch distance to the perfect spiral galaxy M74 hosting three core-collapse supernovae},
author = {Sung Jang, In and Gyoon Lee, Myung, E-mail: isjang@astro.snu.ac.kr, E-mail: mglee@astro.snu.ac.kr},
abstractNote = {M74 (NGC 628) is a famous face-on spiral galaxy, hosting three core-collapse supernovae (SNe): SN Ic 2002ap, SN II-P 2003gd, and SN II-P 2013ej. However, its distance is not well known. We present a distance estimation for this galaxy based on the Tip of the Red Giant Branch (TRGB) method. We obtain photometry of the resolved stars in the arm-free region of M74 from F555W and F814W images in the Hubble Space Telescope archive. The color-magnitude diagram of the resolved stars shows a dominant red giant branch (RGB) as well as blue main sequence stars, red helium burning stars, and asymptotic giant branch stars. The I-band luminosity function of the RGB stars shows the TRGB to be at I {sub TRGB} = 26.13 ± 0.03 mag, and T {sub RGB} = 25.97 ± 0.03. From this, we derive the distance modulus to M74 to be 30.04 ± 0.04 (random) ± 0.12 (systematic) (corresponding to a linear distance of 10.19 ± 0.14 ± 0.56 Mpc). With this distance estimate, we calibrate the standardized candle method for SNe II-P. From the absolute magnitudes of SN 2003gd, we derive a value of the Hubble constant, H {sub 0} = 72 ± 6 (random) ± 7 (systematic) km s{sup –1} Mpc{sup –1}. It is similar to recent estimates based on the luminosity calibration of Type Ia supernovae.},
doi = {10.1088/0004-637X/792/1/52},
journal = {Astrophysical Journal},
number = 1,
volume = 792,
place = {United States},
year = {Mon Sep 01 00:00:00 EDT 2014},
month = {Mon Sep 01 00:00:00 EDT 2014}
}
  • We present a new determination of the distance to M101, host of the Type Ia supernova (SN Ia) 2011fe, based on the tip of the red giant branch (TRGB) method. Our determination is based on Hubble Space Telescope archival F555W and F814W images of nine fields within the galaxy. Color-magnitude diagrams of arm-free regions in all fields show a prominent red giant branch. We measure the I-band magnitudes of the TRGB, obtaining a mean value of I{sub TRGB} = 25.28 {+-} 0.01 (where the error is a standard error), using an edge-detection method. We derive a weighted mean value ofmore » distance modulus (m - M){sub 0} = 29.30 {+-} 0.01(random) {+-} 0.12(systematic), corresponding to a linear distance of 7.24 {+-} 0.03 {+-} 0.40 Mpc. While previous estimates for M101 show a large range (TRGB distances of (m - M){sub 0} = 29.05-29.42 and Cepheid distances of (m - M){sub 0} = 29.04-29.71), our measurements of the TRGB distances for nine fields show a small dispersion of only 0.02. We combine our distance estimate and photometry in the literature to derive absolute peak magnitudes in optical and near-infrared bands of SN 2011fe. Absolute maximum magnitudes of SN 2011fe are {approx}0.2 mag brighter in the optical band and much more in the NIR than the current calibrations of SNe Ia in the literature. From the optical maximum magnitudes of SN 2011fe we obtain a value of the Hubble constant, H{sub 0} = 65.0 {+-} 0.5(random) {+-} 5.7(systematic) km s{sup -1} Mpc{sup -1}, slightly smaller than other recent determinations of H{sub 0}.« less
  • We investigate the utility of the asymptotic giant branch (AGB) and the red giant branch (RGB) as probes of the star formation history (SFH) of the nearby (D = 2.5 Mpc) dwarf irregular galaxy, KKH 98. Near-infrared (near-IR) Keck Laser Guide Star Adaptive Optics (AO) images resolve 592 IR-bright stars reaching over 1 mag below the tip of the RGB. Significantly deeper optical (F475W and F814W) Hubble Space Telescope images of the same field contain over 2500 stars, reaching to the red clump and the main-sequence turnoff for 0.5 Gyr old populations. Compared to the optical color-magnitude diagram (CMD), themore » near-IR CMD shows significantly tighter AGB sequences, providing a good probe of the intermediate-age (0.5-5 Gyr) populations. We match observed CMDs with stellar evolution models to recover the SFH of KKH 98. On average, the galaxy has experienced relatively constant low-level star formation (5 x 10{sup -4} M{sub sun} yr{sup -1}) for much of cosmic time. Except for the youngest main-sequence populations (age <0.1 Gyr), which are typically fainter than the AO data flux limit, the SFH estimated from the 592 IR-bright stars is a reasonable match to that derived from the much larger optical data set. Differences between the optical- and IR-derived SFHs for 0.1-1 Gyr populations suggest that current stellar evolution models may be overproducing the AGB by as much as a factor of 3 in this galaxy. At the depth of the AO data, the IR-luminous stars are not crowded. Therefore, these techniques can potentially be used to determine the stellar populations of galaxies at significantly further distances.« less
  • We present a precise optical and near-infrared determination of the tip of the red giant branch (TRGB) brightness in the Large and Small Magellanic Clouds (respectively, LMC and SMC). The commonly used calibrations of the absolute magnitude of the TRGB lead to an overestimation of the distance to the LMC and SMC in the K band, and an underestimation of the distance in the optical I band for both galaxies. Reported discrepancies are at the level of 0.2 mag, with respect to the very accurate distance determinations to both MCs based on late-type eclipsing binaries. The differential distances between themore » LMC and SMC obtained in the J and K bands, and for the bolometric brightness are consistent with each other, and with the results obtained from eclipsing binaries and other distance indicators.« less
  • Observational data on the five brightest giants in the globular clusters M3, M5, M13, M15, and M92 are compared with theoretically computed data on the helium flash. The theoretical models considered agree with the observations: with increasing metal abundance T/sub eff/(f1) decreases, i.e., the values (B- V)$sub 0$(5), the mean (B-V)$sub 0$ value for the five brightest giants of a cluster (Fig. 3), increase. It is shown that a comparison of the observed mean absolute magnitudes of the five brightest giants of the different clusters, M/ subV/(5), with the computed M/sub bol/(f1) can provide data on bolometric corrections. It ismore » also pointed out that a more complete array of models with computed evolutionary tracks for giants and additional observational data on the masses of giants of different clusters are necessary for a more detailed comparison of theory and observations. (AIP)« less
  • We present distance determinations for two Local Group dwarf spheroidal galaxies, Carina and Fornax, based on the near-infrared magnitudes of the tip of the red giant branch (TRGB). For Carina we derive true distance moduli of 20.09 and 20.13 mag in the J and K bands, respectively, while for Fornax the same distance modulus of 20.84 mag was derived in both filters. The statistical errors of these determinations are of the order of 0.03-0.04 mag, whereas the systematic uncertainties on the distances are 0.12 mag in the J band and 0.14 mag in the K band. The distances obtained frommore » the near-infrared TRGB method in this paper agree very well with those obtained for these two galaxies from optical calibrations of the TRGB method, their horizontal branches, RR Lyrae variables, and the near-infrared magnitudes of their red clumps.« less