Hubble Space TelescopeObservations of the Large Magellanic Cloud Field around SN 1987A: Distance Determination with Red Clump and Tip of the Red Giant Branch Stars

2000 ◽  
Vol 530 (2) ◽  
pp. 738-743 ◽  
Author(s):  
M. Romaniello ◽  
M. Salaris ◽  
S. Cassisi ◽  
N. Panagia
Keyword(s):  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
Distance Determination ◽  
Sn 1987A ◽  
Red Clump ◽  
Red Giant ◽  
Giant Branch Stars

scholarly journals The Magellanic Edges Survey I: Description and first results

2020 ◽  
Vol 497 (3) ◽  
pp. 3055-3075
Author(s):  
L R Cullinane ◽  
A D Mackey ◽  
G S Da Costa ◽  
S E Koposov ◽  
V Belokurov ◽  
...  
Keyword(s):  
Target Selection ◽  
Radial Distance ◽  
Large Magellanic Cloud ◽  
Disc Model ◽  
Observation Strategy ◽  
First Results ◽  
Mass Estimate ◽  
Red Clump ◽  
Red Giant ◽  
Giant Branch Stars

ABSTRACT We present an overview of, and first science results from, the Magellanic Edges Survey (MagES), an ongoing spectroscopic survey mapping the kinematics of red clump and red giant branch stars in the highly substructured periphery of the Magellanic Clouds. In conjunction with Gaia astrometry, MagES yields a sample of ~7000 stars with individual 3D velocities that probes larger galactocentric radii than most previous studies. We outline our target selection, observation strategy, data reduction, and analysis procedures, and present results for two fields in the northern outskirts (>10° on-sky from the centre) of the Large Magellanic Cloud (LMC). One field, located in the vicinity of an arm-like overdensity, displays apparent signatures of perturbation away from an equilibrium disc model. This includes a large radial velocity dispersion in the LMC disc plane, and an asymmetric line-of-sight velocity distribution indicative of motions vertically out of the disc plane for some stars. The second field reveals 3D kinematics consistent with an equilibrium disc, and yields Vcirc = 87.7 ± 8.0 km s−1 at a radial distance of ~10.5 kpc from the LMC centre. This leads to an enclosed mass estimate for the LMC at this radius of (1.8 ± 0.3) × 1010 M⊙.

Distance to SN 1987A and the LMC

1999 ◽  
Vol 190 ◽  
pp. 549-554
Author(s):  
Nino Panagia
Keyword(s):  
Angular Size ◽  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
Light Curves ◽  
Distance Modulus ◽  
Absolute Size ◽  
Sn 1987A

Using the new reductions of the IUE light curves by Sonneborn et al. (1997) and an extensive set of HST images of SN 1987A we have repeated and improved Panagia et al. (1991) analysis to obtain a better determination of the distance to the supernova. In this way we have derived an absolute size of the ringRabs= (6.23 ± 0.08) x 1017cm and an angular sizeR″ = 808 ± 17 mas, which give a distance to the supernovad(SN1987A) = 51.4 ± 1.2 kpc and a distance modulusm–M(SN1987A) = 18.55 ± 0.05. Allowing for a displacement of SN 1987A position relative to the LMC center, the distance to the barycenter of the Large Magellanic Cloud is also estimated to bed(LMC) = 52.0±1.3 kpc, which corresponds to a distance modulus ofm–M(LMC) = 18.58±0.05.

scholarly journals Studies of the large Magellanic Cloud using optical interstellar emission lines

1991 ◽  
Vol 148 ◽  
pp. 421-427
Author(s):  
J. Meaburn
Keyword(s):  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
Emission Lines ◽  
Optical Observations ◽  
Sn 1987A ◽  
30 Doradus

Optical observations have been made of the halo of 30 Doradus, in the vicinity of SN 1987A and of giant shells in the LMC.

scholarly journals AKARI IRC survey of the Large Magellanic Cloud: A new feature in the infrared color—magnitude diagram

2008 ◽  
Vol 4 (S256) ◽  
pp. 9-13
Author(s):  
Yoshifusa Ita ◽  
Takashi Onaka ◽  
Daisuke Kato ◽  
Keyword(s):  
Infrared Camera ◽  
Large Magellanic Cloud ◽  
Emission Feature ◽  
Magellanic Cloud ◽  
Circumstellar Dust ◽  
Red Giants ◽  
Broad Emission ◽  
Magnitude Diagram ◽  
Red Giant ◽  
New Feature

AbstractWe observed an area of 10 deg2 of the Large Magellanic Cloud using the Infrared Camera on board AKARI. The observations were carried out using five imaging filters (3, 7, 11, 15, and 24 μm) and a dispersion prism (2 − 5 μm, λ/Δλ ~ 20) equipped in the IRC. The 11 and 15 μm data, which are unique to AKARI IRC, allow us to construct color-magnitude diagrams that are useful to identify stars with circumstellar dust. We found a new sequence in the color-magnitude diagram, which is attributed to red giants with luminosity fainter than that of the tip of the first red giant branch. We suggest that this sequence is likely to be related to the broad emission feature of aluminium oxide at 11.5 μm.

scholarly journals The Tip of the Red Giant Branch Distance to the Large Magellanic Cloud

2000 ◽  
Vol 119 (3) ◽  
pp. 1197-1204 ◽  
Author(s):  
Shoko Sakai ◽  
Dennis Zaritsky ◽  
Robert C. Kennicutt, Jr.
Keyword(s):  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
Red Giant
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