Large Magellanic Cloud Near-Infrared Synoptic Survey. Ii. The Wesenheit Relations and Their Application to the Distance Scale

Bhardwaj, Anupam; Kanbur, Shashi M.; Macri, Lucas M.; Singh, Harinder P.; Ngeow, Chow-Choong; Wagner-Kaiser, R.; Sarajedini, Ata

doi:10.3847/0004-6256/151/4/88

Cited by 55 publications

(48 citation statements)

References 72 publications

(202 reference statements)

Supporting

Mentioning

Contrasting

Order By: Relevance

“…We use a standard t-test to check the significance of the difference in the slopes of our PL relations with published work. The details of t-test can be found in Ngeow et al (2015) and Bhardwaj et al (2015a). In brief, we calculate T-values using the errors on the slopes and the standard deviation of PL relations.…”

Section: Comparison With Published Pl Relationsmentioning

confidence: 99%

Period–Luminosity relations derived from the OGLE-III first-overtone mode Cepheids in the Magellanic Clouds

Bhardwaj¹,

Ngeow²,

Singh³

2016

Mon. Not. R. Astron. Soc.

Self Cite

View full text Add to dashboard Cite

We present multi-band Period-Luminosity (PL) relations for first-overtone mode Cepheids in the Small Magellanic Cloud (SMC). We derive optical band PL relations and the Wesenheit function using V I mean magnitudes from the Optical Gravitational Lensing Experiment (OGLE-III) survey. We cross-match OGLE-III firstovertone mode Cepheids to the 2MASS and SAGE-SMC catalogs to derive PL relations at near-infrared (JHK s ) and mid-infrared (3.6 & 4.5µm) wavelengths. We test for possible non-linearities in these PL relations using robust statistical tests and find a significant break only in the optical-band PL relations at 2.5 days for first-overtone mode Cepheids. We do not find statistical evidence for a non-linearity in these PL relations at 1 day. The multi-band PL relations for fundamental-mode Cepheids in the SMC also exhibit a break at 2.5 days. We suggest that the period break around 2.5 days is related to sharp changes in the light curve parameters for SMC Cepheids. We also derive new optical and mid-infrared band PL relations for first-overtone mode Cepheids in the Large Magellanic Cloud (LMC). We compare multi-band PL relations for first-overtone mode Cepheids in the Magellanic Clouds and find a significant difference in the slope of the V -band PL relations but not for I-band PL relations. The slope of PL relations are found to be consistent in most of the infrared bands. A relative distance modulus of ∆µ = 0.49 ± 0.02 mag between the two clouds is estimated using multi-band PL relations for the first-overtone mode Cepheids in the SMC and LMC.

show abstract

Section: Comparison With Published Pl Relationsmentioning

confidence: 99%

Period–Luminosity relations derived from the OGLE-III first-overtone mode Cepheids in the Magellanic Clouds

Bhardwaj¹,

Ngeow²,

Singh³

2016

Mon. Not. R. Astron. Soc.

Self Cite

View full text Add to dashboard Cite

show abstract

“…where M H and M K s are predicted by the period-luminosity relation 5 . Figure 4 plots some extinction coefficients in the near IR in the literature and shows a large scatter among them.…”

Section: Impact Of the Uncertainty In The Extinction Lawmentioning

confidence: 99%

“…Its good collection of time-series data for a wide area of the LMC has been producing important results on classical Cepheids and type II Cepheids ( [4][5][6][7]). …”

mentioning

confidence: 99%

See 1 more Smart Citation

Time-series surveys and pulsating stars: The near-infrared perspective

Matsunaga

2017

EPJ Web Conf.

View full text Add to dashboard Cite

Abstract. The purpose of this review is to discuss the advantages and problems of nearinfrared surveys in observing pulsating stars in the Milky Way. One of the advantages of near-infrared surveys, when compared to optical counterparts, is that the interstellar extinction is significantly smaller. As we see in this review, a significant volume of the Galactic disk can be reached by infrared surveys but not by optical ones. Towards highly obscured regions in the Galactic mid-plane, however, the interstellar extinction causes serious problems even with near-infrared data in understanding the observational results. After a review on previous and current near-infrared surveys, we discuss the effects of the interstellar extinction in optical (including Gaia) to near-infrared broad bands based on a simple calculation using synthetic spectral energy distribution. We then review the recent results on classical Cepheids towards the Galactic center and the bulge, as a case study, to see the impact of the uncertainty in the extinction law. The extinction law, i.e. the wavelength dependency of the extinction, is not fully characterized, and its uncertainty makes it hard to make the correction. Its characterization is an urgent task in order to exploit the outcomes of ongoing large-scale surveys of pulsating stars, e.g. for drawing a map of pulsating stars across the Galactic disk.

show abstract

“…In order to minimize the reddening problem, we have used the Wesenheit magnitudes (see, e.g., Majaess et al 2011;Bhardwaj et al 2016) defined here as W K =Ks−0.45× (J − Ks). Selected cuts in the W K versus J−Ks CMD allow us to eliminate most of the background disk stars, retaining distant red giants (Figure 1).…”

Section: Selection Of Globular Cluster Candidatesmentioning

confidence: 99%

New VVV Survey Globular Cluster Candidates in the Milky Way Bulge*

Minniti

Geisler

Alonso-García

et al. 2017

ApJL

View full text Add to dashboard Cite

It is likely that a number of Galactic globular clusters remain to be discovered, especially toward the Galactic bulge. High stellar density combined with high and differential interstellar reddening are the two major problems for finding globular clusters located toward the bulge. We use the deep near-IR photometry of the VISTA Variables in the Vía Láctea (VVV) Survey to search for globular clusters projected toward the Galactic bulge, and hereby report the discovery of 22 new candidate globular clusters. These objects, detected as high density regions in our maps of bulge red giants, are confirmed as globular cluster candidates by their color-magnitude diagrams. We provide their coordinates as well as their near-IR color-magnitude diagrams, from which some basic parameters are derived, such as reddenings and heliocentric distances. The color-magnitude diagrams reveal well defined red giant branches in all cases, often including a prominent red clump. The new globular cluster candidates exhibit a variety of extinctions (0.06 < A Ks < 2.77) and distances (5.3 < D < 9.5 kpc). We also classify the globular cluster candidates into 10 metal-poor and 12 metal-rich clusters, based on the comparison of their colormagnitude diagrams with those of known globular clusters also observed by the VVV Survey. Finally, we argue that the census for Galactic globular clusters still remains incomplete, and that many more candidate globular clusters (particularly the low luminosity ones) await to be found and studied in detail in the central regions of the Milky Way.

show abstract

Large Magellanic Cloud Near-Infrared Synoptic Survey. Ii. The Wesenheit Relations and Their Application to the Distance Scale

Cited by 55 publications

References 72 publications

Period–Luminosity relations derived from the OGLE-III first-overtone mode Cepheids in the Magellanic Clouds

Period–Luminosity relations derived from the OGLE-III first-overtone mode Cepheids in the Magellanic Clouds

Time-series surveys and pulsating stars: The near-infrared perspective

New VVV Survey Globular Cluster Candidates in the Milky Way Bulge*

Contact Info

Product

Resources

About