The VMC Survey: XXXII. Pre-main-sequence populations in the Large Magellanic Cloud

Viktor Zivkov, Joana M. Oliveira, M. Murgia, Monika G. Petr-Gotzens, B. Adebahr, Maria Rosa L. Cioni, Stefano Rubele, Jacco Th Van Loon, Kenji Bekki, Felice Cusano, Richard De Grijs, Valentin D. Ivanov, Marcella Marconi, Florian Niederhofer, Vincenzo Ripepi, Ning Chen Sun

Research output: Contribution to journalReview article

Abstract

Context. Detailed studies of intermediate- and low-mass pre-main-sequence (PMS) stars outside the Galaxy have so far been conducted only for small targeted regions harbouring known star formation complexes. The VISTA Survey of the Magellanic Clouds (VMC) provides an opportunity to study PMS populations down to solar masses on a galaxy-wide scale. Aims. Our goal is to use near-infrared data from the VMC survey to identify and characterise PMS populations down to ∼1 Mo. across the Magellanic Clouds. We present our colour-magnitude diagram method, and apply it to a ∼1.5 deg2 pilot field located in the Large Magellanic Cloud. Methods. The pilot field is divided into equal-size grid elements. We compare the stellar population in every element with the population in nearby control fields by creating Ks/(Y-Ks) Hess diagrams; the observed density excesses over the local field population are used to classify the stellar populations. Results. Our analysis recovers all known star formation complexes in this pilot field (N 44, N 51, N 148, and N 138) and for the first time reveals their true spatial extent. In total, around 2260 PMS candidates with ages ≲ 10 Myr are found in the pilot field. PMS structures, identified as areas with a significant density excess of PMS candidates, display a power-law distribution of the number of members with a slope of -0.86 ± 0.12. We find a clustering of the young stellar populations along ridges and filaments where dust emission in the far-infrared (FIR) (70 μm-500 μm) is bright. Regions with young populations lacking massive stars show a lower degree of clustering and are usually located in the outskirts of the star formation complexes. At short FIR wavelengths (70 μm,100 μm) we report a strong dust emission increase in regions hosting young massive stars, which is less pronounced in regions populated only by less massive (≲ 4 Mo.) PMS stars.

Original languageEnglish
Article numberA143
JournalAstronomy and Astrophysics
Volume620
DOIs
Publication statusPublished - 1 Dec 2018

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Magellanic clouds
young population
diagram
dust
star formation
pre-main sequence stars
power law distribution
massive stars
near infrared
galaxies
wavelength
color-magnitude diagram
complex formation
ridges
filaments
diagrams
grids
slopes
method
wavelengths

Cite this

Zivkov, V., Oliveira, J. M., Murgia, M., Petr-Gotzens, M. G., Adebahr, B., Cioni, M. R. L., ... Sun, N. C. (2018). The VMC Survey: XXXII. Pre-main-sequence populations in the Large Magellanic Cloud. Astronomy and Astrophysics, 620, [A143]. https://doi.org/10.1051/0004-6361/201833951
Zivkov, Viktor ; Oliveira, Joana M. ; Murgia, M. ; Petr-Gotzens, Monika G. ; Adebahr, B. ; Cioni, Maria Rosa L. ; Rubele, Stefano ; Van Loon, Jacco Th ; Bekki, Kenji ; Cusano, Felice ; De Grijs, Richard ; Ivanov, Valentin D. ; Marconi, Marcella ; Niederhofer, Florian ; Ripepi, Vincenzo ; Sun, Ning Chen. / The VMC Survey : XXXII. Pre-main-sequence populations in the Large Magellanic Cloud. In: Astronomy and Astrophysics. 2018 ; Vol. 620.
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abstract = "Context. Detailed studies of intermediate- and low-mass pre-main-sequence (PMS) stars outside the Galaxy have so far been conducted only for small targeted regions harbouring known star formation complexes. The VISTA Survey of the Magellanic Clouds (VMC) provides an opportunity to study PMS populations down to solar masses on a galaxy-wide scale. Aims. Our goal is to use near-infrared data from the VMC survey to identify and characterise PMS populations down to ∼1 Mo. across the Magellanic Clouds. We present our colour-magnitude diagram method, and apply it to a ∼1.5 deg2 pilot field located in the Large Magellanic Cloud. Methods. The pilot field is divided into equal-size grid elements. We compare the stellar population in every element with the population in nearby control fields by creating Ks/(Y-Ks) Hess diagrams; the observed density excesses over the local field population are used to classify the stellar populations. Results. Our analysis recovers all known star formation complexes in this pilot field (N 44, N 51, N 148, and N 138) and for the first time reveals their true spatial extent. In total, around 2260 PMS candidates with ages ≲ 10 Myr are found in the pilot field. PMS structures, identified as areas with a significant density excess of PMS candidates, display a power-law distribution of the number of members with a slope of -0.86 ± 0.12. We find a clustering of the young stellar populations along ridges and filaments where dust emission in the far-infrared (FIR) (70 μm-500 μm) is bright. Regions with young populations lacking massive stars show a lower degree of clustering and are usually located in the outskirts of the star formation complexes. At short FIR wavelengths (70 μm,100 μm) we report a strong dust emission increase in regions hosting young massive stars, which is less pronounced in regions populated only by less massive (≲ 4 Mo.) PMS stars.",
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Zivkov, V, Oliveira, JM, Murgia, M, Petr-Gotzens, MG, Adebahr, B, Cioni, MRL, Rubele, S, Van Loon, JT, Bekki, K, Cusano, F, De Grijs, R, Ivanov, VD, Marconi, M, Niederhofer, F, Ripepi, V & Sun, NC 2018, 'The VMC Survey: XXXII. Pre-main-sequence populations in the Large Magellanic Cloud' Astronomy and Astrophysics, vol. 620, A143. https://doi.org/10.1051/0004-6361/201833951

The VMC Survey : XXXII. Pre-main-sequence populations in the Large Magellanic Cloud. / Zivkov, Viktor; Oliveira, Joana M.; Murgia, M.; Petr-Gotzens, Monika G.; Adebahr, B.; Cioni, Maria Rosa L.; Rubele, Stefano; Van Loon, Jacco Th; Bekki, Kenji; Cusano, Felice; De Grijs, Richard; Ivanov, Valentin D.; Marconi, Marcella; Niederhofer, Florian; Ripepi, Vincenzo; Sun, Ning Chen.

In: Astronomy and Astrophysics, Vol. 620, A143, 01.12.2018.

Research output: Contribution to journalReview article

TY - JOUR

T1 - The VMC Survey

T2 - XXXII. Pre-main-sequence populations in the Large Magellanic Cloud

AU - Zivkov, Viktor

AU - Oliveira, Joana M.

AU - Murgia, M.

AU - Petr-Gotzens, Monika G.

AU - Adebahr, B.

AU - Cioni, Maria Rosa L.

AU - Rubele, Stefano

AU - Van Loon, Jacco Th

AU - Bekki, Kenji

AU - Cusano, Felice

AU - De Grijs, Richard

AU - Ivanov, Valentin D.

AU - Marconi, Marcella

AU - Niederhofer, Florian

AU - Ripepi, Vincenzo

AU - Sun, Ning Chen

PY - 2018/12/1

Y1 - 2018/12/1

N2 - Context. Detailed studies of intermediate- and low-mass pre-main-sequence (PMS) stars outside the Galaxy have so far been conducted only for small targeted regions harbouring known star formation complexes. The VISTA Survey of the Magellanic Clouds (VMC) provides an opportunity to study PMS populations down to solar masses on a galaxy-wide scale. Aims. Our goal is to use near-infrared data from the VMC survey to identify and characterise PMS populations down to ∼1 Mo. across the Magellanic Clouds. We present our colour-magnitude diagram method, and apply it to a ∼1.5 deg2 pilot field located in the Large Magellanic Cloud. Methods. The pilot field is divided into equal-size grid elements. We compare the stellar population in every element with the population in nearby control fields by creating Ks/(Y-Ks) Hess diagrams; the observed density excesses over the local field population are used to classify the stellar populations. Results. Our analysis recovers all known star formation complexes in this pilot field (N 44, N 51, N 148, and N 138) and for the first time reveals their true spatial extent. In total, around 2260 PMS candidates with ages ≲ 10 Myr are found in the pilot field. PMS structures, identified as areas with a significant density excess of PMS candidates, display a power-law distribution of the number of members with a slope of -0.86 ± 0.12. We find a clustering of the young stellar populations along ridges and filaments where dust emission in the far-infrared (FIR) (70 μm-500 μm) is bright. Regions with young populations lacking massive stars show a lower degree of clustering and are usually located in the outskirts of the star formation complexes. At short FIR wavelengths (70 μm,100 μm) we report a strong dust emission increase in regions hosting young massive stars, which is less pronounced in regions populated only by less massive (≲ 4 Mo.) PMS stars.

AB - Context. Detailed studies of intermediate- and low-mass pre-main-sequence (PMS) stars outside the Galaxy have so far been conducted only for small targeted regions harbouring known star formation complexes. The VISTA Survey of the Magellanic Clouds (VMC) provides an opportunity to study PMS populations down to solar masses on a galaxy-wide scale. Aims. Our goal is to use near-infrared data from the VMC survey to identify and characterise PMS populations down to ∼1 Mo. across the Magellanic Clouds. We present our colour-magnitude diagram method, and apply it to a ∼1.5 deg2 pilot field located in the Large Magellanic Cloud. Methods. The pilot field is divided into equal-size grid elements. We compare the stellar population in every element with the population in nearby control fields by creating Ks/(Y-Ks) Hess diagrams; the observed density excesses over the local field population are used to classify the stellar populations. Results. Our analysis recovers all known star formation complexes in this pilot field (N 44, N 51, N 148, and N 138) and for the first time reveals their true spatial extent. In total, around 2260 PMS candidates with ages ≲ 10 Myr are found in the pilot field. PMS structures, identified as areas with a significant density excess of PMS candidates, display a power-law distribution of the number of members with a slope of -0.86 ± 0.12. We find a clustering of the young stellar populations along ridges and filaments where dust emission in the far-infrared (FIR) (70 μm-500 μm) is bright. Regions with young populations lacking massive stars show a lower degree of clustering and are usually located in the outskirts of the star formation complexes. At short FIR wavelengths (70 μm,100 μm) we report a strong dust emission increase in regions hosting young massive stars, which is less pronounced in regions populated only by less massive (≲ 4 Mo.) PMS stars.

KW - Galaxies: Individual: LMC

KW - Galaxies: Star formation

KW - Stars: Pre-main sequence

KW - Stars: Statistics

KW - Techniques: Photometric

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U2 - 10.1051/0004-6361/201833951

DO - 10.1051/0004-6361/201833951

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JO - ASTRONOMY & ASTROPHYSICS

JF - ASTRONOMY & ASTROPHYSICS

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Zivkov V, Oliveira JM, Murgia M, Petr-Gotzens MG, Adebahr B, Cioni MRL et al. The VMC Survey: XXXII. Pre-main-sequence populations in the Large Magellanic Cloud. Astronomy and Astrophysics. 2018 Dec 1;620. A143. https://doi.org/10.1051/0004-6361/201833951