OGLE-ing the Magellanic System: Optical Reddening Maps of the Large and Small Magellanic Clouds from Red Clump Stars

Skowron, D. M.; Skowron, J.; Udalski, A.; Szymański, M. K.; Soszyński, I.; Wyrzykowski, Ł.; Ulaczyk, K.; Poleski, R.; Kozłowski, S.; Pietrukowicz, P.; Mróz, P.; Rybicki, K.; Iwanek, P.; Wrona, Marcin; Gromadzki, M.

doi:10.3847/1538-4365/abcb81

Cited by 102 publications

(87 citation statements)

References 57 publications

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“…Studies in the literature show that 30 Dor and the central region of the LMC have higher reddening compared with the rest of the disc (e.g., Zaritsky et al 2004;Haschke et al 2011;Subramanian & Subramaniam 2013;Górski et al 2020;Skowron et al 2021;Grady et al 2021). Recent extinction maps of Mazzi et al (2021) based on star-formation history (SFH) studies using VMC data also support these previous findings.…”

Section: Impact Of Reddening and Distance Variationsmentioning

confidence: 70%

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The VMC survey – XLIV: mapping metallicity trends in the large magellanic cloud using near-infrared passbands

Choudhury

Grijs

Bekki

et al. 2021

Monthly Notices of the Royal Astronomical Society

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We have derived high-spatial-resolution metallicity maps covering ∼105 deg2 across the Large Magellanic Cloud (LMC) using near-infrared passbands from the VISTA Survey of the Magellanic Clouds. We attempt to understand the metallicity distribution and gradients of the LMC up to a radius of ∼ 6 kpc. We identify red giant branch (RGB) stars in spatially distinct Y, (Y − Ks) colour–magnitude diagrams. In any of our selected subregions, the RGB slope is used as an indicator of the average metallicity, based on calibration to metallicity using spectroscopic data. The mean LMC metallicity is [Fe/H] = −0.42 dex (σ[Fe/H] = 0.04 dex). We find the bar to be mildly metal-rich compared with the outer disc, showing evidence of a shallow gradient in metallicity (−0.008 ± 0.001 dex kpc−1) from the galaxy’s centre to a radius of 6 kpc. Our results suggest that the LMC’s stellar bar is chemically similar to the bars found in large spiral galaxies. The LMC’s radial metallicity gradient is asymmetric. It is metal-poor and flatter towards the southwest, in the direction of the Bridge. This hints at mixing and/or distortion of the spatial metallicity distribution, presumably caused by tidal interactions between the Magellanic Clouds.

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Section: Impact Of Reddening and Distance Variationsmentioning

confidence: 70%

“…Nidever et al (2020) reported metallicities of 3600 RGB stars based on high-resolution H-band spectra from the APOGEE survey. Skowron et al (2021) used the APOGEE data of red giant (RG) stars from Nidever et al (2020) to estimate an LMC MG of −0.026±0.002 dex deg −1 out to around 8 • .…”

mentioning

confidence: 99%

The VMC survey – XLIV: mapping metallicity trends in the large magellanic cloud using near-infrared passbands

Choudhury

Grijs

Bekki

et al. 2021

Monthly Notices of the Royal Astronomical Society

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“…There is the 2019 determination made by reference [81] which measures TRGB in a nine SNIa hosts, adds 5 from [80], and calibrates TRGB in the LMC which yields H 0 = 69.8 ± 0.8(stat) ± 1.7(sys) km s −1 Mpc −1 at 68% CL and reference [82] (F20), for which H 0 = 69.6 ± 0.8(stat) ± 1.7(sys) km s −1 Mpc −1 at 68% CL, or the same but with a different accounting of the LMC extinction of the TRGB using reddening maps derived from red clump stars by [83] gives H 0 = 72.4 ± 2.0 km s −1 Mpc −1 at 68% CL. A value of H 0 ∼ 72 km s −1 Mpc −1 also results from the revised OGLE Team LMC reddening maps [84,85]. The addition of two new TRGB measurements in NGC 1404 and NGC 5643, host to 4 SNIa [86] appears to raise the F20 value of H 0 by ∼1% to ∼70 km s −1 Mpc −1 but the revised value is not tabulated.…”

Section: Latementioning

confidence: 93%

In the realm of the Hubble tension—a review of solutions ^*

Valentino

Mena²,

Pan³

et al. 2021

Class. Quantum Grav.

1,327

760

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The simplest ΛCDM model provides a good fit to a large span of cosmological data but harbors large areas of phenomenology and ignorance. With the improvement of the number and the accuracy of observations, discrepancies among key cosmological parameters of the model have emerged. The most statistically significant tension is the 4σ to 6σ disagreement between predictions of the Hubble constant, H 0, made by the early time probes in concert with the ‘vanilla’ ΛCDM cosmological model, and a number of late time, model-independent determinations of H 0 from local measurements of distances and redshifts. The high precision and consistency of the data at both ends present strong challenges to the possible solution space and demands a hypothesis with enough rigor to explain multiple observations—whether these invoke new physics, unexpected large-scale structures or multiple, unrelated errors. A thorough review of the problem including a discussion of recent Hubble constant estimates and a summary of the proposed theoretical solutions is presented here. We include more than 1000 references, indicating that the interest in this area has grown considerably just during the last few years. We classify the many proposals to resolve the tension in these categories: early dark energy, late dark energy, dark energy models with 6 degrees of freedom and their extensions, models with extra relativistic degrees of freedom, models with extra interactions, unified cosmologies, modified gravity, inflationary models, modified recombination history, physics of the critical phenomena, and alternative proposals. Some are formally successful, improving the fit to the data in light of their additional degrees of freedom, restoring agreement within 1–2σ between Planck 2018, using the cosmic microwave background power spectra data, baryon acoustic oscillations, Pantheon SN data, and R20, the latest SH0ES Team Riess, et al (2021 Astrophys. J. 908 L6) measurement of the Hubble constant (H 0 = 73.2 ± 1.3 km s−1 Mpc−1 at 68% confidence level). However, there are many more unsuccessful models which leave the discrepancy well above the 3σ disagreement level. In many cases, reduced tension comes not simply from a change in the value of H 0 but also due to an increase in its uncertainty due to degeneracy with additional physics, complicating the picture and pointing to the need for additional probes. While no specific proposal makes a strong case for being highly likely or far better than all others, solutions involving early or dynamical dark energy, neutrino interactions, interacting cosmologies, primordial magnetic fields, and modified gravity provide the best options until a better alternative comes along.

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“…For the Gaia photometry, we follow the dereddening procedure of Gaia Collaboration et al (2018a), using the first two terms in their Equation (1) to do so. The recent red clump calibration of Skowron et al (2021) has provided reddening maps for the LMC and SMC with good resolution in the central parts of the Clouds, regions where those of Schlegel et al (1998) suffer from high levels of dust. Consequently, we utilize these recent maps for the innermost regions of the Clouds.…”

Section: Datamentioning

confidence: 99%

Magellanic Mayhem: Metallicities and Motions

Grady

Belokurov

Evans

2021

ApJ

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We assemble a catalog of Magellanic Cloud red giants from Data Release 2 of the Gaia mission and, utilizing machine-learning methods, obtain photometric metallicity estimates for them. In doing so, we are able to chemically map the entirety of the Magellanic System at once. Our maps reveal a plethora of substructure within our red giant sample, with the Large Magellanic Cloud (LMC) bar and spiral arm being readily apparent. We uncover a curious spiral-like feature in the southern portion of the LMC disk, hosting relatively metal-rich giants and likely a by-product of historic encounters with the Small Magellanic Cloud (SMC). Modeling the LMC as an inclined thin disk, we find a shallow metallicity gradient of −0.048 ± 0.001 dex kpc −1 out to ∼12°from the center of the dwarf. We see evidence that the SMC is disrupting, with its outer isodensity contours displaying the S-shape symptomatic of tidal stripping. On studying the proper motions of the SMC giants, we observe a population of them being violently dragged toward the larger Cloud. The perturbed stars predominantly lie in front of the SMC, and we interpret that they exist as a tidal tail of the dwarf, trailing in its motion and undergoing severe disruption from the LMC. We find the metallicity structure in the Magellanic Bridge region to be complex, with evidence for a composite nature in this stellar population, consisting of both LMC and SMC debris.Unified Astronomy Thesaurus concepts: Galaxies (573); Local Group (929); Large Magellanic Cloud (903); Small Magellanic Cloud (1468)

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OGLE-ing the Magellanic System: Optical Reddening Maps of the Large and Small Magellanic Clouds from Red Clump Stars

Cited by 102 publications

References 57 publications

The VMC survey – XLIV: mapping metallicity trends in the large magellanic cloud using near-infrared passbands

The VMC survey – XLIV: mapping metallicity trends in the large magellanic cloud using near-infrared passbands

In the realm of the Hubble tension—a review of solutions ^*

Magellanic Mayhem: Metallicities and Motions

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OGLE-ing the Magellanic System: Optical Reddening Maps of the Large and Small Magellanic Clouds from Red Clump Stars

Cited by 102 publications

References 57 publications

The VMC survey – XLIV: mapping metallicity trends in the large magellanic cloud using near-infrared passbands

The VMC survey – XLIV: mapping metallicity trends in the large magellanic cloud using near-infrared passbands

In the realm of the Hubble tension—a review of solutions *

Magellanic Mayhem: Metallicities and Motions

Contact Info

Product

Resources

About

In the realm of the Hubble tension—a review of solutions ^*