OGLE-ing the Magellanic System: Cepheids in the Bridge*

Jacyszyn-Dobrzeniecka, Anna M.; Soszyński, I.; Udalski, A.; Szymański, M. K.; Skowron, D. M.; Mróz, P.; Kruszyńska, K.; Iwanek, P.; Poleski, R.; Ulaczyk, K.; Rybicki, K.; Wrona, Marcin

doi:10.3847/1538-4357/ab61f1

Cited by 63 publications

(101 citation statements)

References 94 publications

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“…Those calibrations play a fundamental role in the Hubble Constant value determination (Freedman et al 2001;Freedman et al 2019;Riess et al 2016;Yuan et al 2019). Both galaxies are also the subject of stellar populations and 3D structure studies (Ripepi et al 2012;Jacyszyn-Dobrzeniecka et al 2017). In recent years both Magellanic Clouds were the subject of intense scrutiny of the Araucaria Project (Gieren et al 2005), which led to a precise distance determination for both galaxies (Pietrzyński et al 2013;Graczyk et al 2014;Pietrzyński et al 2019), a determination of the Cepheid period-luminosity relation dependence on metallicity ( Wielgórski et al 2017;, the determination of precise fundamental physical parameters of eclipsing binary systems containing red giants (Graczyk et al 2018) and a calibration of a new method to use blue supergiant stars as extragalactic distance indicators (Urbaneja et al 2017).…”

Section: Introductionmentioning

confidence: 99%

Empirical Calibration of the Reddening Maps in the Magellanic Clouds

Górski

Zgirski

Pietrzyński

et al. 2020

ApJ

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We present reddening maps of the Large Magellanic Cloud (LMC) and Small Magellanic Cloud (SMC), based on color measurements of the red clump. Reddening values of our maps were obtained by calculating the difference of the observed and intrinsic color of the red clump in both galaxies. To obtain the intrinsic color of the red clump, we used reddenings obtained from late-type eclipsing binary systems, measurements for blue supergiants and reddenings derived from Strömgren photometry of B-type stars. We obtained intrinsic color of the red clump (V − I) 0 = 0.838 ± 0.034 mag in the LMC, and (V − I) 0 = 0.814 ± 0.034 mag in the SMC. We prepared our map with 3 arcmin resolution,

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Section: Introductionmentioning

confidence: 99%

Empirical Calibration of the Reddening Maps in the Magellanic Clouds

Górski

Zgirski

Pietrzyński

et al. 2020

ApJ

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“…Distance estimations using Classical Cepheids (e.g. Jacyszyn-Dobrzeniecka et al 2016 andRipepi et al 2017) report evidences for an ellipsoidal morphology of the SMC that appears to be very extended along the line of sight, with different depths for different regions and a mean depth of ∼5 kpc (rising to and above ∼20 kpc in some regions). Using RR Lyrae as distance tracers there are observations of similar morphology and depth (e.g.…”

Section: Introductionmentioning

confidence: 99%

“…Using RR Lyrae as distance tracers there are observations of similar morphology and depth (e.g. Jacyszyn-Dobrzeniecka et al 2017 andMuraveva et al 2018) with the SMC's bound structure identified as an ellipsoid with an axes ratio of 1:1.1:3.3 with the main axis roughly along the line of sight. These observations are at odds with the increasing amount of evidence for tidal disruption that would disfavor such an extended bound structure of the SMC.…”

Section: Introductionmentioning

confidence: 99%

Revealing the tidal scars of the Small Magellanic Cloud

Leo

Carrera

Noel

et al. 2020

Monthly Notices of the Royal Astronomical Society

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Due to their close proximity, the Large and Small Magellanic Clouds (LMC/SMC) provide natural laboratories for understanding how galaxies form and evolve. With the goal of determining the structure and dynamical state of the SMC, we present new spectroscopic data for ∼ 3000 SMC red giant branch stars observed using the AAOmega spectrograph at the Anglo-Australian Telescope. We complement our data with further spectroscopic measurements from previous studies that used the same instrumental configuration as well as proper motions from the Gaia Data Release 2 catalogue. Analysing the photometric and stellar kinematic data, we find that the SMC centre of mass presents a conspicuous offset from the velocity centre of its associated H i gas, suggesting that the SMC gas is likely to be far from dynamical equilibrium. Furthermore, we find evidence that the SMC is currently undergoing tidal disruption by the LMC within 2 kpc of the centre of the SMC, and possibly all the way into the very core. This is revealed by a net outward motion of stars from the SMC centre along the direction towards the LMC and an apparent tangential anisotropy at all radii. The latter is expected if the SMC is undergoing significant tidal stripping, as we demonstrate using a suite of N-body simulations of the SMC/LMC system disrupting around the Milky Way. Our results suggest that dynamical models for the SMC that assume a steady state will need to be revisited.

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“…They can be divided into three types based on the pulsation mode: RRab -fundamental mode, RRc -first overtone, and RRd -double mode (fundamental and first overtone) pulsators. The RR Lyrae pulsators are often used as tracers of the properties of the old population of the Galactic halo and bulge (e.g., Dékány et al 2013;Belokurov et al 2018a;Prudil et al 2019a), or nearby galaxies (e.g., Haschke et al 2012a,b;Jacyszyn-Dobrzeniecka et al 2017). In general, these variables are not used as probes of the Galactic disc, although they have been used successfully to put constraints on the structure of the thick disc and the mechanisms that contributed to its formation (Kinemuchi et al 2006;Kinman et al 2009;Mateu et al 2012;Mateu & Vivas 2018;Dékány et al 2018).…”

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confidence: 99%

Evidence for Galactic disc RR Lyrae stars in the solar neighbourhood

Prudil

Dékány

Grebel

et al. 2020

Monthly Notices of the Royal Astronomical Society

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We present a kinematical study of 314 RR Lyrae stars in the solar neighbourhood using the publicly available photometric, spectroscopic, and Gaia DR2 astrometric data to explore their distribution in the Milky Way. We report an overdensity of 22 RR Lyrae stars in the solar neighbourhood at a pericenter distance of between 5-9 kpc from the Galactic center. Their orbital parameters and their chemistry indicate that these 22 variables share the kinematics and the [Fe/H] values of the Galactic disc, with an average metallicity and tangential velocity of [Fe/H]=−0.60 dex and v θ = 241 km s −1 , respectively. From the distribution of the Galactocentric spherical velocity components, we find that these 22 disc-like RR Lyrae variables are not consistent with the Gaia Sausage (Gaia-Enceladus), unlike almost half of the local RR Lyrae stars. Chemical information from the literature shows that the majority of the selected pericenter peak RR Lyrae variables are α-poor, a property shared by typically much younger stars in the thin disc. Using the available photometry we rule out a possible misclassification with the known classical and anomalous Cepheids. The similar kinematic, chemical, and pulsation properties of these disc RR Lyrae stars suggest they share a common origin. In contrast, we find the RR Lyrae stars associated with the Gaia-Enceladus based on their kinematics and chemical composition show a considerable metallicity spread in the old population (∼ 1 dex).

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OGLE-ing the Magellanic System: Cepheids in the Bridge*

Cited by 63 publications

References 94 publications

Empirical Calibration of the Reddening Maps in the Magellanic Clouds

Empirical Calibration of the Reddening Maps in the Magellanic Clouds

Revealing the tidal scars of the Small Magellanic Cloud

Evidence for Galactic disc RR Lyrae stars in the solar neighbourhood

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