The IRSF Magellanic Clouds Point Source Catalog

Kato, Daisuke; Nagashima, Chie; Nagayama, Takahiro; Kurita, Mikio; Koerwer, Joel F.; Kawai, Takeshi; Yamamuro, Tomoyasu; Zenno, Takahiro; Nishiyama, Shogo; Baba, Daisuke; Kadowaki, Ryota; Haba, Y.; Hatano, Hitoshi; Shimizu, Hideyuki; Nishimura, Mamiko; Nagata, T.; Sato, Shuji; Murai, Yuka; Kawazu, T.; Nakajima, Yasushi; Nakaya, Hidehiko; Kandori, Ryo; Kusakabe, Nobuhiko; Ishihara, Akika; Kaneyasu, N.; Hashimoto, Jun; Tamura, Motohide; Tanabé, Toshihiko; Ita, Yoshifusa; Matsunaga, Noriyuki; Nakada, Y.; Sugitani, Koji; Wakamatsu, K.; Glass, Ian S.; Feast, M. W.; Menzies, John; Whitelock, P. A.; Fourie, P.A.; Stoffels, J.; Evans, Geoff; Hasegawa, Tetsuo

doi:10.1093/pasj/59.3.615

Cited by 230 publications

(111 citation statements)

References 24 publications

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“…Standard stars from Persson et al (1998) were observed on each night and the results presented here are on the natural system of the SIRIUS camera, but with the zero-point of the Persson et al standards. These magnitudes are expected to be close to those on the Two Micron All Sky Survey (2MASS) system (Kato et al 2007). The field of view is 7.8 × 7.8 arcmin 2 , but this is reduced to 7.2 × 7.2 arcmin 2 during the course of the reductions.…”

Section: O B S E Rvat I O N Ssupporting

confidence: 54%

Asymptotic giant branch stars in the Phoenix dwarf galaxy

Menzies¹,

Feast²,

Whitelock³

et al. 2008

Monthly Notices RAS

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JHK s near‐infrared photometry of stars in the Phoenix dwarf galaxy is presented and discussed. Combining these data with the optical photometry of Massey et al. allows a rather clean separation of field stars from Phoenix members. The discovery of a Mira variable (P= 425 d), which is almost certainly a carbon star, leads to an estimate of the distance modulus of 23.10 ± 0.18 that is consistent with other estimates and indicates the existence of a significant population of age ∼2 Gyr. The two carbon stars of Da Costa have Mbol=−3.8 and are consistent with belonging to a population of similar age; some other possible members of such a population are identified. A Da Costa non‐carbon star is ΔKs∼ 0.3 mag brighter than these two carbon stars. It may be an asymptotic giant branch star of the dominant old population. The nature of other stars lying close to it in the Ks, (J−Ks) diagram needs studying.

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Section: O B S E Rvat I O N Ssupporting

confidence: 54%

Asymptotic giant branch stars in the Phoenix dwarf galaxy

Menzies¹,

Feast²,

Whitelock³

et al. 2008

Monthly Notices RAS

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“…Bonanos et al (2009Bonanos et al ( , 2010 took advantage of the new data and compiled catalogs by starting with all massive stars in the LMC and SMC with high quality spectral classifications, and then matching them to entries in the Spitzer and other photometric data bases. The catalogs contain U , B, V , and I from various sources and JHK photometry (primarily from the Two Micron All Sky Survey, 2MASS; Skrutskie et al 2006 and the targeted IRSF survey, (Kato et al 2007) In this paper, we concentrate on a sub-sample of the Bonanos et al (2009Bonanos et al ( , 2010 catalogs, namely those O stars which are also in the Blair et al (2009) FUSE sample. This will allow direct comparison of results derived from different diagnostics in many cases.…”

Section: The Sample and Datamentioning

confidence: 99%

Mass-loss rates from mid-infrared excesses in LMC and SMC O stars

Massa¹,

Fullerton²,

Prinja³

2017

Monthly Notices of the Royal Astronomical Society

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We use a combination of BV JHK and Spitzer [3.6], [5.8] and [8.0] photometry to determine IR excesses for a sample of 58 LMC and 46 SMC O stars. This sample is ideal for determining IR excesses because the very small line of sight reddening minimizes uncertainties due to extinction corrections. We use the core-halo model developed by Lamers & Waters (1984a) to translate the excesses into mass loss rates and demonstrate that the results of this simple model agree with the more sophisticated CMFGEN models to within a factor of 2. Taken at face value, the derived mass loss rates are larger than those predicted by Vink et al. (2001), and the magnitude of the disagreement increases with decreasing luminosity. However, the IR excesses need not imply large mass loss rates. Instead, we argue that they probably indicate that the outer atmospheres of O stars contain complex structures and that their winds are launched with much smaller velocity gradients than normally assumed. If this is the case, it could affect the theoretical and observational interpretations of the "weak wind" problem, where classical mass loss indicators suggest that the mass loss rates of lower luminosity O stars are far less than expected.

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“…The USNO-B1 catalog source has R1, B2, and R2 plate magnitudes of 17.76, 21.46, and 18.9 mag, respectively. The IRSF Magellanic Cloud point source catalog (Kato et al 2007) has a source with J and H magnitudes of 18.37 ± 0.07 and  18.62 0.25 mag, respectively. The last source is from the Guide Star Catalog (V2.3) which has red, green and 0.8 μm photographic band magnitudes of 18.54, 17.69 and 18.52, respectively.…”

Section: Nova Positionmentioning

confidence: 99%

Pan-Chromatic Observations of the Remarkable Nova Large Magellanic Cloud 2012

Schwarz

Shore

Page

et al. 2015

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We present the results of an intensive multiwavelength campaign on nova LMC 2012. This nova evolved very rapidly in all observed wavelengths. The time to fall two magnitudes in the V band was only 2 days. In X-rays the super soft phase began 13 ± 5 days after discovery and ended around day 50 after discovery. During the super soft phase, the Swift/XRT and Chandra spectra were consistent with the underlying white dwarf (WD) being very hot, ∼1 MK, and luminous, ∼10 38 erg s −1 . The UV, optical, and near-IR photometry showed a periodic variation after the initial and rapid fading had ended. Timing analysis revealed a consistent 19.24 ± 0.03 hr period in all UV, optical, and near-IR bands with amplitudes of ∼0.3 mag which we associate with the orbital period of the central binary. No periods were detected in the corresponding X-ray data sets. A moderately high inclination system, i = 60 ± 10, was inferred from the early optical emission lines. The HST/STIS UV spectra were highly unusual with only the N V (1240 Å) line present and superposed on a blue continuum. The lack of emission lines and the observed UV and optical continua from four epochs can be fit with a low mass ejection event, ∼10 −6  M , from a hot and massive WD near the Chandrasekhar limit. The WD, in turn, significantly illuminated its subgiant companion which provided the bulk of the observed UV/optical continuum emission at the later dates. The inferred extreme WD characteristics and low mass ejection event favor nova LMC 2012 being a recurrent nova of the U Sco subclass.

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The IRSF Magellanic Clouds Point Source Catalog

Cited by 230 publications

References 24 publications

Asymptotic giant branch stars in the Phoenix dwarf galaxy

Asymptotic giant branch stars in the Phoenix dwarf galaxy

Mass-loss rates from mid-infrared excesses in LMC and SMC O stars

Pan-Chromatic Observations of the Remarkable Nova Large Magellanic Cloud 2012

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