Using Photometry to Probe the Circumstellar Environment of Δ Scorpii

Jones, C. E.; Wiegert, Paul; Tycner, C.; Henry, Gregory W.; Cyr, R. P.; Halonen, R. J.; Muterspaugh, Matthew W.

doi:10.1088/0004-6256/145/5/142

Cited by 18 publications

(27 citation statements)

References 34 publications

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“…We take the Galactocentric cylindrical coordinate system (R, Φ, Z) to characterize the Galactic dust distribution, where R is the Galactocentric radius, Φ is the position angle and Z is the vertical distance. We assume that the dust distribution is axisymmetric and can be parameterized by an exponential disk (Misiriotis et al 2006;Jones et al 2011)…”

Section: Methodsmentioning

confidence: 99%

“…For the stellar thin disk, the general conclusion is that it can be fitted by an exponential disk with scale-length 2.6 ± 0.5 kpc and scale-height 220 ∼ 450 pc. For the dust component, it has been shown that, despite of spiral arms, flares and warps (Drimmel & Spergel 2001;Marshall et al 2006;Amôres & Lépine 2005;Reylé et al 2009), the global distribution of dust also follows an exponential disk (Misiriotis et al 2006;Jones et al 2011). However, the scale-length and scale-height of the dust disk have not been constrained very well yet.…”

Section: Introductionmentioning

confidence: 99%

“…Drimmel & Spergel (2001) presented a three-dimensional Galactic dust distribution model and obtained a scale-length of 2.26 kpc and scale-height of 134.4 pc by fitting the FIR data from COBE/DIRBE, while Misiriotis et al (2006) got the results of 5.0 kpc and 100 pc respectively also by modeling FIR emission of COBE data. Jones et al (2011) created a three-dimensional Galactic extinction map using the spectra of more than 56,000 M dwarfs in SDSS (Sloan Digital Sky Survey, York et al 2000) and then obtianed the dust scale-height of 119 pc around solar region. To get a more reliable modeling of Galactic dust distribution, a larger sample of dust extinction tracer is better.…”

Section: Introductionmentioning

confidence: 99%

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Three-dimensional Structure of the Milky Way Dust: Modeling of LAMOST Data

Shen

Hou

et al. 2018

ApJ

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We present a three-dimensional modeling of the Milky Way dust distribution by fitting the value-added star catalog of LAMOST spectral survey. The global dust distribution can be described by an exponential disk with scale-length of 3,192 pc and scale height of 103 pc. In this modeling, the Sun is located above the dust disk with a vertical distance of 23 pc. Besides the global smooth structure, two substructures around the solar position are also identified. The one located at 150 • < l < 200 • and −5 • < b < −30 • is consistent with the Gould Belt model of Gontcharov (2009), and the other one located at 140 • < l < 165 • and 0 • < b < 15 • is associated with the Camelopardalis molecular clouds.

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Section: Methodsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Three-dimensional Structure of the Milky Way Dust: Modeling of LAMOST Data

Shen

Hou

et al. 2018

ApJ

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“…This can partially explain the observed scatter. In addition, the dust scale height is 120 pc (Jones et al 2011). First, this can explain the large differential reddening within the bulge.…”

Section: Far Disk Source?mentioning

confidence: 97%

UKIRT-2017-BLG-001Lb: A Giant Planet Detected through the Dust

Shvartzvald

Novati

Gaudi

et al. 2018

ApJL

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We report the discovery of a giant planet in event UKIRT-2017-BLG-001, detected by the UKIRT microlensing survey. The mass ratio between the planet and its host is q = 1.50 +0.17 −0.14 × 10 −3 , about 1.5 times the Jupiter/Sun mass ratio. The event lies 0.35 • from the Galactic center and suffers from high extinction of A K = 1.68. Therefore, it could be detected only by a near-infrared survey. The field also suffers from large spatial differential extinction, which makes it difficult to estimate the source properties required to derive the angular Einstein radius. Nevertheless, we find evidence suggesting that the source is located in the far disk. If correct, this would be the first source star of a microlensing event to be identified as belonging to the far disk. We estimate the lens mass and distance using a Bayesian analysis to find that the planet's mass is 1.28 +0.37 −0.44 M J , and it orbits a 0.81 +0.21 −0.27 M star at an instantaneous projected separation of 4.18 +0.96 −0.88 AU. The system is at a distance of 6.3 +1.6 −2.1 kpc, and so likely resides in the Galactic bulge. In addition, we find a non-standard extinction curve in this field, in agreement with previous results toward high-extinction fields near the Galactic center. Subject headings: gravitational lensing: micro -Galaxy: bulge-binaries: general -planetary systems 8 Based on the extinctions of red clump stars measured by Nidever et al. (2012), the current WFIRST fields have quartile K s extinctions of 0.38 and 0.64.

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“…These corrections rely on column densities calculated from 100 and 240 µm Galactic emission along the line-of-sight out to infinity, and therefore may overestimate the true extinction to nearby stars. Jones et al (2011) provides a more robust Galactic extinction map by fitting extinction curves to the fluxes of ∼56,000 M dwarfs in the spectral range 5700-9200Å from the W11 catalog. We correct for extinction using the method of Jones et al (2011), except for M dwarfs not present in the Jones et al (2011) catalog, where we apply the extinction corrections of Schlegel et al (1998).…”

Section: Initial Samplementioning

confidence: 99%

Runaway M Dwarf Candidates From the Sloan Digital Sky Survey

Favia

West

Theissen

2015

ApJ

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We present a sample of 20 runaway M dwarf candidates (RdMs) within 1 kpc of the Sun whose Galactocentric velocities exceed 400 km s −1 . The candidates were selected from the SDSS DR7 M Dwarf Catalog of West et al. (2011). Our RdMs have SDSS+USNO-B proper motions that are consistent with those recorded in the PPMXL, LSPM, and combined WISE +SDSS+2MASS catalogs. Sixteen RdMs are classified as dwarfs, while the remaining four RdMs are subdwarfs. We model the Galactic potential using a bulge-disk-halo profile (Kenyon et al. 2008;Brown et al. 2014). Our fastest RdM, with Galactocentric velocity 658.5 ± 236.9 km s −1 , is a possible hypervelocity candidate, as it is unbound in 77% of our simulations. About half of our RdMs have kinematics that are consistent with ejection from the Galactic center. Seven of our RdMs have kinematics consistent with an ejection scenario from M31 or M32 to within 2σ, although our distance-limited survey makes such a realization unlikely. No more than four of our RdMs may have originated from the Leo stream. We propose that to within measurement errors, most of our bound RdMs are likely disk runaways or halo objects, and may have been accelerated through a series of multi-body interactions within the Galactic disk or possibly supernovae explosions.

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Using Photometry to Probe the Circumstellar Environment of Δ Scorpii

Cited by 18 publications

References 34 publications

Three-dimensional Structure of the Milky Way Dust: Modeling of LAMOST Data

Three-dimensional Structure of the Milky Way Dust: Modeling of LAMOST Data

UKIRT-2017-BLG-001Lb: A Giant Planet Detected through the Dust

Runaway M Dwarf Candidates From the Sloan Digital Sky Survey

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