Three-Dimensional Maps of the Magellanic Clouds Using Rr Lyrae Stars and Cepheids. Ii. The Small Magellanic Cloud

Haschke, Raoul; Grebel, Eva K.; Duffau, S.

doi:10.1088/0004-6256/144/4/107

Cited by 85 publications

(68 citation statements)

References 63 publications

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“…Therefore, it is not too surprising that the RC shape in the central region of the SMC looks quite regular and any deviations become visible only at larger radius. We note that the central SMC RR Lyrae also show little spatial pattern or variations and have a depth of only ∼8 kpc, similar to what we observe in our western fields (Haschke et al 2012).…”

Section: Discussionsupporting

confidence: 86%

“…OGLE-IV (Kozlowski et al 2013) will provide high-quality time-series photometry with which RR Lyrae and Cepheids can be identified and accurate distances measured, as was done by Haschke et al (2012) with OGLE-III. OGLE-IV, SkyMapper (Keller et al 2012) and DES (Abbott et al 2012), as well as other DECam programs, will provide photometry to well below the SMC HB over a large area of the MCs and with which RC stars can be exploited to study the three-dimensional structure of the SMC.…”

Section: Discussionmentioning

confidence: 99%

“…Several studies in the 1980s found a large line-of-sight depth in the central SMC using young Cepheids (Mathewson et al 1986(Mathewson et al , 1988, with Caldwell & Coulson (1986) finding hints of two arms in the southwest. Haschke et al (2012) used multiepoch Optical Gravitational Lensing Experiment-III (OGLE-III; Udalski et al 2008) photometry to study the three-dimensional (3D) distribution of cepheids (∼30-300 Myr old) and RR Lyrae ( 10 Gyr old) stars in the inner SMC (R < 2 • ). While both populations are found to have an extended scale height, the older stars have a fairly homogeneous distribution whereas the young stars are in an inclined orientation that is closer in the northeast than in the southwest.…”

Section: Introductionmentioning

confidence: 99%

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A Tidally Stripped Stellar Component of the Magellanic Bridge

Nidever

Monachesi

Bell

et al. 2013

ApJ

111

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Deep photometry of the Small Magellanic Cloud (SMC) stellar periphery (R = 4 • , 4.2 kpc) is used to study its line-of-sight depth with red clump (RC) stars. The RC luminosity function is affected little by young ( 1 Gyr) blue-loop stars in these regions because their main-sequence counterparts are not observed in the color-magnitude diagrams. The SMCs eastern side is found to have a large line-of-sight depth (∼23 kpc) while the western side has a much shallower depth (∼10 kpc), consistent with previous photographic plate photometry results. We use a model SMC RC luminosity function to deconvolve the observed RC magnitudes and construct the density function in distance for our fields. Three of the eastern fields show a distance bimodality with one component at the "systemic" ∼67 kpc SMC distance and a second component at ∼55 kpc. Our data are not reproduced well by the various extant Magellanic Cloud and Stream simulations. However, the models predict that the known H i Magellanic Bridge (stretching from the SMC eastward toward the Large Magellanic Cloud, LMC) has a decreasing distance with angle from the SMC and should be seen in both the gaseous and stellar components. From comparison with these models, we conclude that the most likely explanation for our newly identified ∼55 kpc stellar structure in the eastern SMC is a stellar counterpart of the H i Magellanic Bridge that was tidally stripped from the SMC ∼200 Myr ago during a close encounter with the LMC. This discovery has important implications for microlensing surveys of the SMC.

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Section: Discussionsupporting

confidence: 86%

Section: Discussionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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A Tidally Stripped Stellar Component of the Magellanic Bridge

Nidever

Monachesi

Bell

et al. 2013

ApJ

111

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“…Compared to the LMC, the SMC has a much greater depth and, while there is some evidence for a flattened distribution of young stars (e.g., Haschke et al 2012b), the parameters are relatively uncertain. Because of this and the relatively small number of associated radio pulsars, we have chosen a simple model for the SMC, a spherical Gaussian nebula centered at (a SMC ,…”

Section: Dmentioning

confidence: 99%

“…We fix = A 3000 SMC pc based on the distribution of Cepheid variables (Haschke et al 2012b) and fit for n SMC 0 .…”

Section: Dmentioning

confidence: 99%

A New Electron-Density Model for Estimation of Pulsar and FRB Distances

Yao¹,

Manchester²,

Wang³

2017

ApJ

1,055

997

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We present a new model for the distribution of free electrons in the Galaxy, the Magellanic Clouds, and the intergalactic medium (IGM) that can be used to estimate distances to real or simulated pulsars and fast radio bursts (FRBs) based on their dispersion measure (DM). The Galactic model has an extended thick disk representing the so-called warm interstellar medium, a thin disk representing the Galactic molecular ring, spiral arms based on a recent fit to Galactic H II regions, a Galactic Center disk, and seven local features including the Gum Nebula, Galactic Loop I, and the Local Bubble. An offset of the Sun from the Galactic plane and a warp of the outer Galactic disk are included in the model. Parameters of the Galactic model are determined by fitting to 189 pulsars with independently determined distances and DMs. Simple models are used for the Magellanic Clouds and the IGM. Galactic model distances are within the uncertainty range for 86 of the 189 independently determined distances and within 20% of the nearest limit for a further 38 pulsars. We estimate that 95% of predicted Galactic pulsar distances will have a relative error of less than a factor of 0.9. The predictions of YMW16 are compared to those of the TC93 and NE2001 models showing that YMW16 performs significantly better on all measures. Timescales for pulse broadening due to interstellar scattering are estimated for (real or simulated) Galactic and Magellanic Cloud pulsars and FRBs.

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