Annual Parallax Determination Toward a New X-Ray-Emitting Class 0 Candidate With the Water Maser in the NGC 2264 Star-Forming Region

Kamezaki, Tatsuya; Imura, Kenji; Omodaká, Toshihiro; Handa, Toshihiro; Tsuboi, Y.; Nagayama, Tomonori; Hirota, Tomoya; Sunada, Kazuyoshi; Kobayashi, Hideyuki; Chibueze, James O.; Kawai, Eiji; Nakano, Makoto

doi:10.1088/0067-0049/211/2/18

Cited by 29 publications

(25 citation statements)

References 48 publications

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“…The Sung et al (1997) distance is in good agreement with a recent VLBI distance for a maser source in the cluster (d = 738 +57 −50 pc; Kamezaki et al 2014) and with a recent analysis of data for a newly identified NGC 2264 pre-main sequence EB (d = 756 ± 96 pc; Gillen et al 2014). …”

Section: Physical Properties Of the Short-duration Flux Dip Classsupporting

confidence: 89%

Csi 2264: Characterizing Young Stars in NGC 2264 With Short-Duration Periodic Flux Dips in Their Light Curves

Stauffer

Cody

McGinnis

et al. 2015

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We identify nine young stellar objects (YSOs) in the NGC 2264 star-forming region with optical CoRoT light curves exhibiting short-duration, shallow periodic flux dips. All of these stars have infrared excesses that are consistent with their having inner disk walls near the Keplerian co-rotation radius. The repeating photometric dips have FWHMs generally less than 1 day, depths almost always less than 15%, and periods (3 < P < 11 days) consistent with dust near the Keplerian co-rotation period. The flux dips vary considerably in their depth from epoch to epoch, but usually persist for several weeks and, in two cases, were present in data collected in successive years. For several of these stars, we also measure the photospheric rotation period and find that the rotation and dip periods are the same, as predicted by standard "disk-locking" models. We attribute these flux dips to clumps of material in or near the inner disk wall, passing through our line of sight to the stellar photosphere. In some cases, these dips are also present in simultaneous Spitzer IRAC light curves at 3.6 and 4.5 microns. We characterize the properties of these dips, and compare the stars with light curves exhibiting this behavior to other classes of YSOs in NGC 2264. A number of physical mechanisms could locally increase the dust scale height near the inner disk wall, and we discuss several of those mechanisms; the most plausible mechanisms are either a disk warp due to interaction with the stellar magnetic field or dust entrained in funnel-flow accretion columns arising near the inner disk wall.

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Section: Physical Properties Of the Short-duration Flux Dip Classsupporting

confidence: 89%

Csi 2264: Characterizing Young Stars in NGC 2264 With Short-Duration Periodic Flux Dips in Their Light Curves

Stauffer

Cody

McGinnis

et al. 2015

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“…Parallax and proper motion data and fits for G213.70−12.60. References (23)(24)(25)(26)(27)(28)(29)(30)(31)(32)(33)(34)(35)(36)(37)(38)(39) Correlated data from both groups of bands were divided into separate data files, corrected for ionospheric delays using total electron content models, and residual multi-band delays were determined for all sources. Dispersive "ionosphere-only" delays were formed by differencing the delays at 4.3 and 7.3 GHz, and then scaled to 6.7 GHz.…”

Section: Supplementary Materialsmentioning

confidence: 99%

The local spiral structure of the Milky Way

et al. 2016

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“…It is worth mentioning that not all molecular gas in Figure 9 is interacting with SNR G205.5+0.5. For ex-ample, the bule part in the upper-right corner of Figure 9, which belongs to the NGC 2264 GMC complex and is located at a distance of ∼ 740-900 pc (e.g., Sung et al 1997;Baxter et al 2009;Kamezaki et al 2014) is probably not related to the SNR.…”

Section: Snr G2055+05 (Monoceros Nebula)mentioning

confidence: 99%

Molecular Environments of Three Large Supernova Remnants in the Third Galactic Quadrant: G205.5+0.5, G206.9+2.3, and G213.0–0.6

Zhou

Yang

et al. 2017

ApJ

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We present CO observations toward three large supernova remnants (SNRs) in the third Galactic quadrant using the Purple Mountain Observatory Delingha 13.7 m millimeter-wavelength telescope. The observations are part of the high-resolution CO survey of the Galactic plane between Galactic longitudes l = −10• to 250• and latitudes b = −5• to 5• . CO emission was detected toward the three SNRs: G205.5+0.5 (Monoceros Nebula), G206.9+2.3 (PKS 0646+06), and G213.0−0.6. Both of SNRs G205.5+0.5 and G213.0−0.6 exhibit the morphological agreement (or spatial correspondences) between the remnant and the surrounding molecular clouds (MCs), as well as kinematic signatures of shock perturbation in the molecular gas. We confirm that the two SNRs are physically associated with their ambient MCs and the shock of SNRs is interacting with the dense, clumpy molecular gas. SNR G206.9+2.3, which is close to the northeastern edge of the Monoceros Nebula, displays the spatial coincidence with molecular partial shell structures at V LSR ∼ 15 km s −1 . While no significant line broadening has been detected within or near the remnant, the strong morphological correspondence between the SNR and the molecular cavity implies that SNR G206.9+2.3 is probably associated with the CO gas and is evolving in the low-density environment. The physical features of individual SNRs, together with the relationship between SNRs and their nearby objects, are also discussed.

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Annual Parallax Determination Toward a New X-Ray-Emitting Class 0 Candidate With the Water Maser in the NGC 2264 Star-Forming Region

Cited by 29 publications

References 48 publications

Csi 2264: Characterizing Young Stars in NGC 2264 With Short-Duration Periodic Flux Dips in Their Light Curves

Csi 2264: Characterizing Young Stars in NGC 2264 With Short-Duration Periodic Flux Dips in Their Light Curves

The local spiral structure of the Milky Way

Molecular Environments of Three Large Supernova Remnants in the Third Galactic Quadrant: G205.5+0.5, G206.9+2.3, and G213.0–0.6

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