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The Astrophysical Distance Scale III: Distance to the Local Group Galaxy

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The Astrophysical Distance Scale III: Distance to the Local Group Galaxy Draft version December 9, 2020 Typeset using LATEX twocolumn style in AASTeX63 The Astrophysical Distance Scale III: Distance to the Local Group Galaxy WLM using Multi-Wavelength Observations of the Tip of the Red Giant Branch, Cepheids, and JAGB Stars Abigail J. Lee,1 Wendy L. Freedman,1 Barry F. Madore,1, 2 Kayla A. Owens,1 Andrew J. Monson,3 and Taylor J. Hoyt1 1Department of Astronomy & Astrophysics, University of Chicago, 5640 South Ellis Avenue, Chicago, IL 60637 2Observatories of the Carnegie Institution for Science 813 Santa Barbara St., Pasadena, CA 91101 3Department of Astronomy & Astrophysics, Pennsylvania State University, 525 Davey Lab, University Park, PA 16802 ABSTRACT The local determination of the Hubble Constant sits at a crossroad. Current estimates of the local expansion rate of the Universe differ by about 1.7-σ, derived from the Cepheid and TRGB based calibrations, applied to type Ia supernovae. To help elucidate possible sources of systematic error causing the tension, we show in this study the recently developed distance indicator, the J-region Asymptotic Giant Branch (JAGB) method (Madore & Freedman 2020), can serve as an independent cross-check and comparison with other local distance indicators. Furthermore, we make the case that the JAGB method has substantial potential as an independent, precise and accurate calibrator of type Ia supernovae for the determination of H0. Using the Local Group galaxy, WLM we present distance comparisons between the JAGB method, a TRGB measurement at near-infrared (JHK) wavelengths, a TRGB measurement in the optical I band, and a multi-wavelength Cepheid period-luminosity relation determination. We find: µ0 (JAGB) = 24:97 0:02 (stat) 0:04 (sys) mag ± ± µ0 (T RGBNIR) = 24:98 0:04 (stat) 0:07 (sys) mag ± ± µ0 (T RGBF 814W ) = 24:93 0:02 (stat) 0:06 (sys) mag ± ± µ0 (Cepheids) = 24:98 0:03 (stat) 0:04 (sys) mag ± ± All four methods are in good agreement, confirming the local self-consistency of the four distance scales at the 3% level, and adding confidence that the JAGB method is as accurate and as precise a distance indicator as either of the other three astrophysically-based methods. Keywords: distance scale { stars: Population II { galaxies: individual (WLM) { galaxies: stellar content { stars: AGB and post-AGB { stars: carbon { stars: variables: Cepheids { cosmology: observations arXiv:2012.04536v1 [astro-ph.CO] 8 Dec 2020 1. INTRODUCTION type Ia supernovae, would provide a more secure de- Measuring both precise and accurate distances to termination of H0 in the nearby universe, and a better galaxies persists as a challenging problem in astronomy. understanding of the magnitude and significance of the Attempts to discover, develop and refine new distance current tension between local (late-time) values of H0 indicator techniques in the past two decades have only and those derived from (early-time) cosmological mod- increased as the need for greater accuracy has grown. eling of cosmic microwave background (CMB) observa- One goal of these endeavors, a robust calibration of tions. Resolving the Hubble tension will require hav- ing systematic effects constrained at the 1-2% percent- level (or better) in their individual accuracies. The two [email protected] current front-runners for high-precision measurements of local distances are the Tip of the Red Giant Branch 2 Lee et al. (TRGB) method used by the Carnegie-Chicago Hub- its on their absolute magnitudes and color, making them ble Program (CCHP) (Freedman et al. 2019, 2020), and distinct and easily identified in color-magnitude space. Cepheid Period-Luminosity based method (the Leavitt For a more comprehensive review of the dredge-up the- Law) used by the Hubble Space Telescope Key Project for ory for carbon stars, see Habing & Olofsson(2003). the past 30 years (Freedman et al. 2001, 2012) and more A review of carbon stars by Battinelli & Demers recently by the SHoES group (Riess et al. 2016; Riess (2005) demonstrated that the mean luminosity of the et al. 2019). Currently however, these two local (TRGB distribution of JAGB stars is relatively constant from vs Cepheid) measurements of H0 differ by almost 1.7-σ, galaxy to galaxy, and preliminary tests carried out by and this tension continues. Is there an independent dis- Freedman & Madore(2020) have also demonstrated the tance indicator, equal in precision and accuracy to the JAGB absolute magnitude has little, if any, dependence Cepheids and TRGB methods, that can serve as a cross- on metallicity or age. Empirically, the mean of the check to shed light on differences in systematics between JAGB luminosity distribution has all of the necessary the two more classical methods? We are now exploring attributes of an excellent distance indicator. that possibility. Both the TRGB and JAGB methods provide a stan- The aim of this paper is to further develop an inde- dard candle. To compare the two methods, Freedman & pendent distance calibrator, the near-infrared J-region Madore(2020) measured and compiled distances to 14 Asymptotic Giant Branch (JAGB) method, recently galaxies, and found the TRGB and JAGB distances to (re)introduced into the distance scale arena (Madore & be in good agreement. However, this study was based Freedman 2020; Freedman & Madore 2020; Ripoche et on previously-published data, not optimized for the de- al. 2020). JAGB stars are Thermally-Pulsating Asymp- tection of JAGB stars. No studies to date have com- totic Giant Branch (TP-AGB) stars with considerable pared distance moduli using both the optical and near- amounts of carbon in their atmospheres (i.e., carbon- infrared TRGB and the JAGB method derived from the to-oxygen ratios of C/O> 1) (Habing & Olofsson 2003). same dataset, using self-consistent processing, calibra- JAGB stars also undergo `dredge-up' events, where with tion and analysis procedures. Accordingly, in this study each thermal pulse the convective envelope penetrates we undertake just such an in-depth study of the galaxy into deeper and deeper layers of the star's interior. Dur- Wolf-Lundmark-Melotte (WLM). ing the third dredge-up phase (and beyond), the con- WLM is a dwarf irregular galaxy located in the outer vective envelope of the star penetrates deep enough edges of the Local Group (Wolf 1909; Melotte 1926). We that it encounters carbon, produced by the He-burning have measured its distance modulus using the TRGB shell, and brings that enriched material to the surface in both the near-infrared JHK bands and optical I (see Habing & Olofsson(2003) for a general review and band, a multi-wavelength Cepheid period-luminosity re- Marigo & Girardi(2007); Marigo et al.(2017) for de- lation determination, and the JAGB method in the J tailed descriptions of TP-AGB evolution). band. We have obtained high-precision ground-based For the younger, more massive AGB stars (1:6 108 data, which we have calibrated using archival HST ob- × years), the temperature at the bottom of the convective servations for the optical and Two-Micron All-Sky Sur- envelope becomes so hot that during the third dredge-up vey (2MASS) data (Skrutskie et al. 2006) for the near phase, the recently-formed carbon is quickly converted infrared. into nitrogen before it can be convected to the surface. The first goal of this paper is to test the degree to This places an upper limit on the luminosity of a JAGB which the JAGB method can be used as a cross check star (Iben 1973; Sackmann et al. 1974). For older, less and comparison with other local distance indicators, massive AGB stars, the third dredge-up phase (and be- such as Cepheids and the TRGB, in order to reveal po- yond) becomes ineffective in transporting carbon to the tentially obfuscated systematics. The second goal of this surface. This imposes a lower limit on the luminosities of paper is to demonstrate that with future development stars entering the JAGB region (Iben & Renzini 1983). and testing, using both ground-based and space-based These theoretical limits are reflected in the observed data, the JAGB method is a distance indicator that is properties JAGB stars, which are well-defined in their comparable to the TRGB and Cepheids in accuracy and near-infrared (NIR) colors and luminosities. JAGB stars precision, and can eventually become the basis for an in- are redder and quite distinct from the bluer oxygen-rich dependent determination of the Hubble Constant. AGB stars, especially at near and mid-infrared wave- Our paper outline is as follows. In Section2, we lengths: a direct result of the large amounts of carbon describe the imaging datasets and the data-reduction in their atmospheres (Marigo & Girardi 2007). Thus, methods used in this study. In Section3, we give a JAGB stars have been observed to have well-defined lim- brief overview of the multi-wavelength application of the Distances to WLM 3 TRGB method, and then present our measurements of The location of this pointing relative to the 8 IMACS the distance modulus to WLM in the near-infrared and chips is shown in Figure1. The STScI processed and independently in the optical. In Section4, we explain charge-transfer-efficiency-corrected and flat-fielded indi- the newly developed JAGB method, and then give our vidual frames (the .flc data type) were pulled from the measured distance modulus. In Section5, we calculate Mikulski Archive for Space Telescopes (MAST). We cor- a Cepheid-based distance modulus, as well as compare rected for pixel-to-pixel geometric distortions caused by our TRGB distance moduli and JAGB distance modulus the optical design of the ACS camera by multiplying values with previous measurements for WLM. Finally, each image by its respective Pixel Area Map, which was we state our conclusions and look to the future with the pulled from the stsci.skypac module.1 JAGB method in Section6.
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