The VMC survey - XXV. The 3D structure of the Small Magellanic Cloud from Classical Cepheids

Vincenzo Ripepi, Maria-Rosa L. Cioni, Maria Ida Moretti, Marcella Marconi, Kenji Bekki, Gisella Clementini, Richard de Grijs, Jim Emerson, Martin A. T. Groenewegen, Valentin D. Ivanov, Roberto Molinaro, Tatiana Muraveva, Joana M. Oliveira, Andres E. Piatti, Smitha Subramanian, Jacco Th. van Loon

Research output: Contribution to journalArticle

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Abstract

The VISTA near-infrared YJK(s) survey of the Magellanic System (VMC) is collecting deep K-s-band time-series photometry of pulsating stars hosted by the two Magellanic Clouds and their connecting bridge. Here, we present Y, J, K-s light curves for a sample of 717 Small Magellanic Cloud (SMC) Classical Cepheids (CCs). These data, complemented with our previous results and V magnitude from literature, allowed us to construct a variety of period-luminosity and period-Wesenheit relationships, valid for Fundamental, First and Second Overtone pulsators. These relations provide accurate individual distances to CCs in the SMC over an area of more than 40 deg(2). Adopting literature relations, we estimated ages and metallicities for the majority of the investigated pulsators, finding that (i) the age distribution is bimodal, with two peaks at 120 +/- 10 and 220 +/- 10 Myr; (i) the more metal-rich CCs appear to be located closer to the centre of the galaxy. Our results show that the three-dimensional distribution of the CCs in the SMC is not planar but heavily elongated for more than 25-30 kpc approximately in the east/north-east towards south-west direction. The young and old CCs in the SMC show a different geometric distribution. Our data support the current theoretical scenario predicting a close encounter or a direct collision between the Clouds some 200 Myr ago and confirm the presence of aCounter-Bridge predicted by some models. The high-precision three-dimensional distribution of young stars presented in this paper provides a new test bed for future models exploring the formation and evolution of the Magellanic System.

Original languageEnglish
Pages (from-to)808-827
Number of pages20
JournalMonthly Notices of the Royal Astronomical Society
Volume472
Issue number1
DOIs
Publication statusPublished - Nov 2017

Cite this

Ripepi, Vincenzo ; Cioni, Maria-Rosa L. ; Moretti, Maria Ida ; Marconi, Marcella ; Bekki, Kenji ; Clementini, Gisella ; de Grijs, Richard ; Emerson, Jim ; Groenewegen, Martin A. T. ; Ivanov, Valentin D. ; Molinaro, Roberto ; Muraveva, Tatiana ; Oliveira, Joana M. ; Piatti, Andres E. ; Subramanian, Smitha ; van Loon, Jacco Th. / The VMC survey - XXV. The 3D structure of the Small Magellanic Cloud from Classical Cepheids. In: Monthly Notices of the Royal Astronomical Society. 2017 ; Vol. 472, No. 1. pp. 808-827.
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abstract = "The VISTA near-infrared YJK(s) survey of the Magellanic System (VMC) is collecting deep K-s-band time-series photometry of pulsating stars hosted by the two Magellanic Clouds and their connecting bridge. Here, we present Y, J, K-s light curves for a sample of 717 Small Magellanic Cloud (SMC) Classical Cepheids (CCs). These data, complemented with our previous results and V magnitude from literature, allowed us to construct a variety of period-luminosity and period-Wesenheit relationships, valid for Fundamental, First and Second Overtone pulsators. These relations provide accurate individual distances to CCs in the SMC over an area of more than 40 deg(2). Adopting literature relations, we estimated ages and metallicities for the majority of the investigated pulsators, finding that (i) the age distribution is bimodal, with two peaks at 120 +/- 10 and 220 +/- 10 Myr; (i) the more metal-rich CCs appear to be located closer to the centre of the galaxy. Our results show that the three-dimensional distribution of the CCs in the SMC is not planar but heavily elongated for more than 25-30 kpc approximately in the east/north-east towards south-west direction. The young and old CCs in the SMC show a different geometric distribution. Our data support the current theoretical scenario predicting a close encounter or a direct collision between the Clouds some 200 Myr ago and confirm the presence of aCounter-Bridge predicted by some models. The high-precision three-dimensional distribution of young stars presented in this paper provides a new test bed for future models exploring the formation and evolution of the Magellanic System.",
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author = "Vincenzo Ripepi and Cioni, {Maria-Rosa L.} and Moretti, {Maria Ida} and Marcella Marconi and Kenji Bekki and Gisella Clementini and {de Grijs}, Richard and Jim Emerson and Groenewegen, {Martin A. T.} and Ivanov, {Valentin D.} and Roberto Molinaro and Tatiana Muraveva and Oliveira, {Joana M.} and Piatti, {Andres E.} and Smitha Subramanian and {van Loon}, {Jacco Th.}",
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Ripepi, V, Cioni, M-RL, Moretti, MI, Marconi, M, Bekki, K, Clementini, G, de Grijs, R, Emerson, J, Groenewegen, MAT, Ivanov, VD, Molinaro, R, Muraveva, T, Oliveira, JM, Piatti, AE, Subramanian, S & van Loon, JT 2017, 'The VMC survey - XXV. The 3D structure of the Small Magellanic Cloud from Classical Cepheids' Monthly Notices of the Royal Astronomical Society, vol. 472, no. 1, pp. 808-827. https://doi.org/10.1093/mnras/stx2096

The VMC survey - XXV. The 3D structure of the Small Magellanic Cloud from Classical Cepheids. / Ripepi, Vincenzo; Cioni, Maria-Rosa L.; Moretti, Maria Ida; Marconi, Marcella; Bekki, Kenji; Clementini, Gisella; de Grijs, Richard; Emerson, Jim; Groenewegen, Martin A. T.; Ivanov, Valentin D.; Molinaro, Roberto; Muraveva, Tatiana; Oliveira, Joana M.; Piatti, Andres E.; Subramanian, Smitha; van Loon, Jacco Th.

In: Monthly Notices of the Royal Astronomical Society, Vol. 472, No. 1, 11.2017, p. 808-827.

Research output: Contribution to journalArticle

TY - JOUR

T1 - The VMC survey - XXV. The 3D structure of the Small Magellanic Cloud from Classical Cepheids

AU - Ripepi, Vincenzo

AU - Cioni, Maria-Rosa L.

AU - Moretti, Maria Ida

AU - Marconi, Marcella

AU - Bekki, Kenji

AU - Clementini, Gisella

AU - de Grijs, Richard

AU - Emerson, Jim

AU - Groenewegen, Martin A. T.

AU - Ivanov, Valentin D.

AU - Molinaro, Roberto

AU - Muraveva, Tatiana

AU - Oliveira, Joana M.

AU - Piatti, Andres E.

AU - Subramanian, Smitha

AU - van Loon, Jacco Th.

PY - 2017/11

Y1 - 2017/11

N2 - The VISTA near-infrared YJK(s) survey of the Magellanic System (VMC) is collecting deep K-s-band time-series photometry of pulsating stars hosted by the two Magellanic Clouds and their connecting bridge. Here, we present Y, J, K-s light curves for a sample of 717 Small Magellanic Cloud (SMC) Classical Cepheids (CCs). These data, complemented with our previous results and V magnitude from literature, allowed us to construct a variety of period-luminosity and period-Wesenheit relationships, valid for Fundamental, First and Second Overtone pulsators. These relations provide accurate individual distances to CCs in the SMC over an area of more than 40 deg(2). Adopting literature relations, we estimated ages and metallicities for the majority of the investigated pulsators, finding that (i) the age distribution is bimodal, with two peaks at 120 +/- 10 and 220 +/- 10 Myr; (i) the more metal-rich CCs appear to be located closer to the centre of the galaxy. Our results show that the three-dimensional distribution of the CCs in the SMC is not planar but heavily elongated for more than 25-30 kpc approximately in the east/north-east towards south-west direction. The young and old CCs in the SMC show a different geometric distribution. Our data support the current theoretical scenario predicting a close encounter or a direct collision between the Clouds some 200 Myr ago and confirm the presence of aCounter-Bridge predicted by some models. The high-precision three-dimensional distribution of young stars presented in this paper provides a new test bed for future models exploring the formation and evolution of the Magellanic System.

AB - The VISTA near-infrared YJK(s) survey of the Magellanic System (VMC) is collecting deep K-s-band time-series photometry of pulsating stars hosted by the two Magellanic Clouds and their connecting bridge. Here, we present Y, J, K-s light curves for a sample of 717 Small Magellanic Cloud (SMC) Classical Cepheids (CCs). These data, complemented with our previous results and V magnitude from literature, allowed us to construct a variety of period-luminosity and period-Wesenheit relationships, valid for Fundamental, First and Second Overtone pulsators. These relations provide accurate individual distances to CCs in the SMC over an area of more than 40 deg(2). Adopting literature relations, we estimated ages and metallicities for the majority of the investigated pulsators, finding that (i) the age distribution is bimodal, with two peaks at 120 +/- 10 and 220 +/- 10 Myr; (i) the more metal-rich CCs appear to be located closer to the centre of the galaxy. Our results show that the three-dimensional distribution of the CCs in the SMC is not planar but heavily elongated for more than 25-30 kpc approximately in the east/north-east towards south-west direction. The young and old CCs in the SMC show a different geometric distribution. Our data support the current theoretical scenario predicting a close encounter or a direct collision between the Clouds some 200 Myr ago and confirm the presence of aCounter-Bridge predicted by some models. The high-precision three-dimensional distribution of young stars presented in this paper provides a new test bed for future models exploring the formation and evolution of the Magellanic System.

KW - stars: oscillations

KW - stars: variables: Cepheids

KW - stars: variables: RR Lyrae

KW - Magellanic Clouds

KW - galaxies: structure

KW - RR LYRAE STARS

KW - FORMATION HISTORY

KW - VARIABLE STARS.

KW - MILKY-WAY

KW - STELLAR POPULATIONS

KW - THEORETICAL-MODELS

KW - OGLE COLLECTION

KW - LIGHT CURVES

KW - RED GIANTS

KW - SYSTEM

U2 - 10.1093/mnras/stx2096

DO - 10.1093/mnras/stx2096

M3 - Article

VL - 472

SP - 808

EP - 827

JO - Monthly Notices of the Royal Astronomical Society

JF - Monthly Notices of the Royal Astronomical Society

SN - 0035-8711

IS - 1

ER -