NEAR-INFRARED PHOTOMETRY OF FOUR STELLAR CLUSTERS IN THE SMALL MAGELLANIC CLOUD

Abstract We have demonstrated the advantage of combining multi-wavelength observations, from the ultraviolet (UV) to near-infrared, to study Kron 3, a massive star cluster in the Small Magellanic Cloud. We have estimated the radius of the cluster Kron 3 to be 2${_{.}^{\prime}}$0 and for the first time, we report the identification of NUV-bright red clump (RC) stars and the extension of the RC in colour and magnitude in the NUV versus (NUV−optical) colour-magnitude diagram (CMD). We found that extension of the RC is an intrinsic property of the cluster and it is not due to contamination of field stars or differential reddening across the field. We studied the spectral energy distribution of the RC stars, and estimated a small range in temperature ∼5000–5500 K, luminosity ∼60–90 L⊙ and radius ∼8.0–11.0 R⊙ supporting their RC nature. The range of UV magnitudes amongst the RC stars (∼23.3 to 24.8 mag) is likely caused by the combined effects of variable mass loss, variation in initial helium abundance (Yini = 0.23 to 0.28), and a small variation in age (6.5-7.5 Gyr) and metallicity ([Fe/H] = −1.5 to −1.3). Spectroscopic follow-up observations of RC stars in Kron 3 are necessary to confirm the cause of the extended RC.

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SPITZERSAGE-SMC INFRARED PHOTOMETRY OF MASSIVE STARS IN THE SMALL MAGELLANIC CLOUD

The Astronomical Journal ◽

10.1088/0004-6256/140/2/416 ◽

2010 ◽

Vol 140 (2) ◽

pp. 416-429 ◽

Cited By ~ 106

Author(s):

A. Z. Bonanos ◽

D. J. Lennon ◽

F. Köhlinger ◽

J. Th. van Loon ◽

D. L. Massa ◽

...

Keyword(s):

Massive Stars ◽

Magellanic Cloud ◽

Small Magellanic Cloud ◽

Infrared Photometry

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Near-Infrared photometry of the LMC cluster Reticulum

International Astronomical Union Colloquium ◽

10.1017/s0252921100010605 ◽

2004 ◽

Vol 193 ◽

pp. 189-192

Author(s):

M. Dall’Ora ◽

G. Bono ◽

J. Storm ◽

V. Ripepi ◽

V. Testa ◽

...

Keyword(s):

Data Reduction ◽

Near Infrared ◽

Large Magellanic Cloud ◽

Magellanic Cloud ◽

Distance Estimate ◽

Infrared Photometry ◽

Rr Lyrae Stars ◽

Rr Lyrae ◽

Lyrae Stars

AbstractWe present U, B, V, I (SUSI@NTT) and J,Ks (SOFI@NTT) photometry of the Large Magellanic Cloud (LMC) cluster Reticulum. The observing strategy and data reduction (DAOPHOTII/ALLFRAME) allowed us to reach an accuracy of the order of 0.01 – 0.03 mag in all the bands at limiting magnitudes typical of RR Lyrae stars. Reticulum hosts a sizable sample of RR Lyrae stars (32), and we supply an accurate distance estimate using the RR Lyrae K-band Period-Luminosity-Metallicity (PLZK) relation. This method presents several advantages when compared with the MV vs [Fe/H] relation, since it is only marginally affected by off-ZAHB evolutionary effects and reddening corrections.

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AGB Stars in the Large Magellanic Cloud as Seen with DeNIS

Symposium - International Astronomical Union ◽

10.1017/s0074180900118352 ◽

1999 ◽

Vol 190 ◽

pp. 385-386 ◽

Cited By ~ 3

Author(s):

M. R. Cioni ◽

H. J. Habing ◽

C. Loup ◽

N. Epchtein ◽

the DeNIS Consortium

Keyword(s):

Near Infrared ◽

Large Magellanic Cloud ◽

Magellanic Cloud ◽

Agb Stars ◽

Infrared Photometry ◽

Sky Survey ◽

Right Ascension

We present infrared photometry of LMC stars taken from a region of 2.5° in right ascension from the DeNIS (Deep Near Infrared Southern Sky Survey) survey.

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THE ARAUCARIA PROJECT. THE DISTANCE OF THE LARGE MAGELLANIC CLOUD FROM NEAR-INFRARED PHOTOMETRY OF RR LYRAE VARIABLES

The Astronomical Journal ◽

10.1088/0004-6256/136/1/272 ◽

2008 ◽

Vol 136 (1) ◽

pp. 272-279 ◽

Cited By ~ 37

Author(s):

Olaf Szewczyk ◽

Grzegorz Pietrzyński ◽

Wolfgang Gieren ◽

Jesper Storm ◽

Alistair Walker ◽

...

Keyword(s):

Near Infrared ◽

Large Magellanic Cloud ◽

Magellanic Cloud ◽

Infrared Photometry ◽

Rr Lyrae

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The Near Infrared Properties of Selected WN Stars in the Large Magellanic Cloud

Symposium - International Astronomical Union ◽

10.1017/s0074180900028928 ◽

1982 ◽

Vol 99 ◽

pp. 231-235

Author(s):

N. Panagia ◽

E.G. Tanzi ◽

M. Tarenghi

Keyword(s):

Near Infrared ◽

Large Magellanic Cloud ◽

Magellanic Cloud ◽

Infrared Photometry ◽

Central Object ◽

30 Doradus

We report here on preliminary infrared photometry of six WN stars in the Large Magellanic Cloud. Besides R136, the central object of the 30 Doradus Nebula, the sample includes three stars (R139, R140, R145) located near the center of the region (within ∼ 1 arcmin) and two more stars (R144, R147) at a distance of ∼ 5 arcmin from R136.

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Morphology of the Small Magellanic Cloud using multiwavelength photometry of classical Cepheids

Monthly Notices of the Royal Astronomical Society ◽

10.1093/mnras/stz2328 ◽

2019 ◽

Vol 489 (3) ◽

pp. 3725-3738 ◽

Cited By ~ 1

Author(s):

Sukanta Deb ◽

Kerdaris Kurbah ◽

Harinder P Singh ◽

Shashi M Kanbur ◽

Chow-Choong Ngeow ◽

...

Keyword(s):

Near Infrared ◽

Weighted Average ◽

Major Axis ◽

Magellanic Cloud ◽

Triaxial Ellipsoid ◽

Distance Modulus ◽

Viewing Angle ◽

Small Magellanic Cloud ◽

Distance Measurements ◽

Classical Cepheids

ABSTRACT This is the second of a series related to the study of geometry of the Magellanic Clouds based on multiwavelength photometry of classical Cepheids. In this paper we determine the geometrical and viewing angle parameters of the Small Magellanic Cloud (SMC) using the Leavitt law for classical Cepheids with/without a break in the law at a certain period as reported in the literature. The study utilizes photometric data for more than 3400 common classical Cepheids (Fundamental (FU) and First overtone (FO)) in optical (V, I), near-infrared (Y, J, Ks) and mid-infrared ([3.6] and [4.5] μm) photometric bands. We obtain statistical reddening and distance modulus free from the effect of reddening to each of the individual Cepheids with respect to the mean distance modulus and reddening of the SMC. The reddening maps of the SMC obtained from the analyses with/without breaks in the Leavitt law show good agreement with each other as well as with other maps available in the literature. The Cartesian coordinates of individual stars with respect to the galaxy plane are obtained using the information of equatorial coordinates (α, δ) as well as extinction-free distance measurements. Modelling the observed 3D distribution of the Cepheids as a triaxial ellipsoid, we obtain the geometrical and viewing angle parameters of the SMC. The weighted average yields the following values of parameters for the SMC: the geometrical axes ratios of 1.000 ± 0.001: 1.544 ± 0.002: 9.742 ± 0.030 and the viewing angle parameters having inclination angle i = 3${^{\circ}_{.}}$465 ± 0${^{\circ}_{.}}$030 with respect to the longest axis from the line of sight and position angle of line of nodes (major axis) θlon = 63${^{\circ}_{.}}$086 ± 0${^{\circ}_{.}}$117.

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A near-infrared VISTA of the Small Magellanic Cloud

Proceedings of the International Astronomical Union ◽

10.1017/s1743921318006828 ◽

2018 ◽

Vol 14 (S344) ◽

pp. 53-56

Author(s):

Maria-Rosa L. Cioni ◽

Florian Niederhofer ◽

Stefano Rubele ◽

Ning-Chen Sun

Keyword(s):

Near Infrared ◽

Stellar Populations ◽

Magellanic Cloud ◽

Magellanic Clouds ◽

Level Of Detail ◽

Star Formation History ◽

Main Body ◽

Small Magellanic Cloud ◽

Formation History ◽

The Galaxy

AbstractVISTA observed the Small Magellanic Cloud (SMC), as part of the VISTA survey of the Magellanic Clouds system (VMC), for six years (2010–2016). The acquired multi-epoch YJKs images have allowed us to probe the stellar populations to an exceptional level of detail across an unprecedented wide area in the near-infrared. This contribution highlights the most recent VMC results obtained on the SMC focusing, in particular, on the clustering of young stellar populations, on the proper motion of stars in the main body of the galaxy and on the spatial distribution of the star formation history.

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Kinematic complexity around NGC 419: resolving the proper motion of the cluster, the Small Magellanic Cloud, and the Magellanic bridge

Monthly Notices of the Royal Astronomical Society ◽

10.1093/mnras/staa3497 ◽

2020 ◽

Vol 500 (2) ◽

pp. 2012-2019

Author(s):

Davide Massari ◽

Silvia Raso ◽

Mattia Libralato ◽

Andrea Bellini

Keyword(s):

Proper Motion ◽

Hubble Space Telescope ◽

Tangential Direction ◽

Magellanic Cloud ◽

Stellar Clusters ◽

Small Magellanic Cloud ◽

Proper Motions ◽

Kinematic Feature ◽

First Time ◽

Magellanic System

ABSTRACT We present Hubble Space Telescope proper motions in the direction of the star cluster NGC 419 in the Small Magellanic Cloud. Because of the high precision of our measurements, for the first time it is possible to resolve the complex kinematics of the stellar populations located in the field, even along the tangential direction. In fact, the proper motions we measured allow us to separate cluster stars, which move on average with ($\mu _{\alpha }\cos \delta ^{\rm NGC\, 419}, \mu _{\delta }^{\rm NGC\, 419}$) = (+0.878 ± 0.055, −1.246 ± 0.048) mas yr−1, from those of the Small Magellanic Cloud and those belonging to a third kinematic feature that we recognize as part of the Magellanic Bridge. Resolving such a kinematic complexity enables the construction of decontaminated colour–magnitude diagrams, as well as the measurement of the absolute proper motion of the three separate components. Our study therefore sets the first steps towards the possibility of dynamically investigating the Magellanic system by exploiting the resolved kinematics of its stellar clusters.

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