The VMC survey – XXVI. Structure of the Small Magellanic Cloud from RR Lyrae stars

Muraveva, T.; Subramanian, Smitha; Clementini, G.; Cioni, M. R. L.; Palmer, M.; Loon, Jacco Th. van; Moretti, M. I.; Grijs, Richard de; Molinaro, R.; Ripepi, V.; Marconi, M.; Emerson, J. P.; Ivanov, V. D.

doi:10.1093/mnras/stx2514

Cited by 75 publications

(93 citation statements)

References 63 publications

(110 reference statements)

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“…This was already hinted at by , briefly mentioned in Belokurov & Erkal (2019, fig. 3 where the gradient in the proper motions is evident) and implied by the smaller distance measured for the Eastern regions of the SMC (Subramanian & Subramaniam 2012;Deb et al 2015;Ripepi et al 2017;Muraveva et al 2018) as they are being pulled towards the LMC and thus closer to us. This last point is corroborated by the gradient seen in Fig.…”

Section: Tidal Disruption Of the Smcmentioning

confidence: 84%

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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Section: Tidal Disruption Of the Smcmentioning

confidence: 84%

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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“…Ripepi et al (2017) also found that young and old Cepheids have different geometric distributions in the SMC. They observed that closer Cepheids are preferentially distributed in the eastern regions of the SMC which are off-centred in the direction of LMC owing to the tidal interaction between the two clouds (Muraveva et al 2018).…”

Section: Spatio-temporal Distributionmentioning

confidence: 99%

“…This repeated interaction between LMC and gas-rich SMC lead to episodic star formations in these two dwarf galaxies which are locked in tidal interaction. It is believed that the Magellanic Bridge and the Magellanic Stream might have formed due to such interactions in the past between the two segments of the MCs (Besla et al 2010;Muraveva et al 2018). As a consequence of these frequent encounters, the tidal stripping of stars and gas/material from the gaseous disk takes place in the Magellanic System.…”

Section: Age Distributionmentioning

confidence: 99%

Reddening map and recent star formation in the Magellanic Clouds based on OGLE IV Cepheids

Joshi

Panchal

2019

A&A

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Context. The reddening maps of the Large Magellanic Cloud (LMC) and Small Magellanic Cloud (SMC) are constructed using the Cepheid Period-Luminosity (P-L) relations. Aims. We examine reddening distribution across the LMC and SMC through largest data on Classical Cepheids provided by the OGLE Phase IV survey. We also investigate the age and spatio-temporal distributions of Cepheids to understand the recent star formation history in the LMC and SMC. Methods. The V and I band photometric data of 2476 fundamental mode (FU) and 1775 first overtone mode (FO) Cepheids in the LMC and 2753 FU and 1793 FO Cepheids in the SMC are analyzed for their P-L relations. We convert period of FO Cepheids to corresponding period of FU Cepheids before combining the two modes of Cepheids. Both galaxies are divided into small segments and combined FU and FO P-L diagrams are drawn in two bands for each segment. The reddening analysis is performed on 133 segments covering a total area of about 154.6 deg 2 in the LMC and 136 segments covering a total area of about 31.3 deg 2 in the SMC. By comparing with well calibrated P-L relations of these two galaxies, we determine reddening E(V − I) in each segment and equivalent reddening E(B − V) assuming the normal extinction law. The period-age relations are used to derive the age of the Cepheids.Results. Using reddening values in different segments across the LMC and SMC, reddening maps are constructed. We find clumpy structures in the reddening distributions of the LMC and SMC. From the reddening map of the LMC, highest reddening of E(V − I) = 0.466 mag is traced in the region centered at α ∼ 85 o .13, δ ∼ −69 o .34 which is in close vicinity of the star forming HII region 30 Doradus. In the SMC, maximum reddening of E(V − I) = 0.189 mag is detected in the region centered at α ∼ 12 o .10, δ ∼ −73 o .07. The mean reddening values in the LMC and SMC are estimated as E(V − I) LMC = 0.113 ± 0.060 mag, E(B − V) LMC = 0.091 ± 0.050 mag, E(V − I) S MC = 0.049 ± 0.070 mag, and E(B − V) S MC = 0.038 ± 0.053 mag.Conclusions. The LMC reddening map displays heterogeneous distribution having small reddening in the central region and higher reddening towards eastern side of the LMC bar. The SMC have relatively small reddening in peripheral regions but larger reddening towards south-west region. In these galaxies, we see an evidence of a common enhanced Cepheid population at around 200 Myr ago which appears to have occurred due to close encounter between the two clouds.

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“…Coppola et al 2011;Sollima et al 2006;Braga et al 2015), and in nearby galaxies (e.g. Moretti et al 2014;Karczmarek et al 2015;Muraveva et al 2018a).…”

Section: Introductionmentioning

confidence: 99%

Standard Galactic field RR Lyrae II: a Gaia DR2 calibration of the period–Wesenheit–metallicity relation

Neeley

Marengo

Freedman

et al. 2019

Monthly Notices of the Royal Astronomical Society

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RR Lyrae stars have long been popular standard candles, but significant advances in methodology and technology have been made in recent years to increase their precision as distance indicators. We present multi-wavelength (optical UBV R c I c and Gaia G, BP, RP; near-infrared JHK s ; mid-infrared [3.6], [4.5]) period-luminosity-metallicity (PLZ), period-Wesenheit-metallicity (PWZ) relations, calibrated using photometry obtained from The Carnegie RR Lyrae Program and parallaxes from the Gaia second data release for 55 Galactic field RR Lyrae stars. The metallicity slope, which has long been predicted by theoretical relations, can now be measured in all passbands. The scatter in the PLZ relations is on the order of 0.2 mag, and is still dominated by uncertainties in the parallaxes. As a consistency check of our PLZ relations, we also measure the distance modulus to the globular cluster M4, the Large Magellanic Cloud (LMC) and the Small Magellanic Cloud (SMC), and our results are in excellent agreement with estimates from previous studies. † Hubble Fellow distances cannot be measured with the traditional distance scale.

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The VMC survey – XXVI. Structure of the Small Magellanic Cloud from RR Lyrae stars

Cited by 75 publications

References 63 publications

Revealing the tidal scars of the Small Magellanic Cloud

Revealing the tidal scars of the Small Magellanic Cloud

Reddening map and recent star formation in the Magellanic Clouds based on OGLE IV Cepheids

Standard Galactic field RR Lyrae II: a Gaia DR2 calibration of the period–Wesenheit–metallicity relation

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