J/AJ/162/279 421 YSOs in of IC 1396 with UKIRT/WFCAM (Silverberg+, 2021)
What's behind the Elephant's trunk? Identifying young stellar objects on the
outskirts of IC 1396.
Silverberg S.M., Gunther H.M., Kim J.S., Principe D.A., Wolk S.J.
<Astron. J., 162, 279-279 (2021)>
=2021AJ....162..279S 2021AJ....162..279S (SIMBAD/NED BibCode)
ADC_Keywords: Nebulae; YSOs; Photometry, infrared; Optical; X-ray sources;
Parallaxes, trigonometric
Keywords: Protoplanetary disks; Young star clusters; Young stellar objects
X-ray astronomy; X-ray point sources; Star-forming regions
Abstract:
Empirically, the estimated lifetime of a typical protoplanetary disk
is <5-10Myr. However, the disk lifetimes required to produce a variety
of observed exoplanetary systems may exceed this timescale. Some
hypothesize that this inconsistency is due to estimating disk
fractions at the cores of clusters, where radiation fields external to
a star-disk system can photoevaporate the disk. To test this, we have
observed a field on the western outskirts of the IC1396 star-forming
region with XMM-Newton to identify new Class III YSO cluster members.
Our X-ray sample is complete for YSOs down to 1.8M☉. We use a
subset of these X-ray sources that have near- and mid-infrared
counterparts to determine the disk fraction for this field. We find
that the fraction of X-ray-detected cluster members that host disks in
the field we observe is 17-7+10%(1σ), comparable with the
29-3+4% found in an adjacent field centered on the cometary
globule IC1396A. We reevaluate YSO identifications in the IC1396A
field using Gaia parallaxes compared to previous color-cut-only
identifications, finding that incorporating independent distance
measurements provides key additional constraints. Given the existence
of at least one massive star producing an external radiation field in
the cluster core, the lack of a statistically significant difference
in disk fraction in each observed field suggests that disk lifetimes
remain consistent as a function of distance from the cluster core.
Description:
A square degree of IC1396 was monitored with the Wide-Field Camera
(WFCAM) on the United Kingdom Infrared Telescope over 21 epochs from
2014 July 18 to 2016 July 12.
We retrieved photometry of the region observed in the UKIRT data from
the early third data release from ESA's Gaia mission (Gaia EDR3), the
AllWISE catalog of data from the Wide-field Infrared Survey Explorer
(WISE), and various pointed observations with the Spitzer Space
Telescope, obtained via the Spitzer Heritage Archive.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table2.dat 305 421 YSOs in the XMM-Newton field of view
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See also:
VII/233 : The 2MASS Extended sources (IPAC/UMass, 2003-2006)
I/337 : Gaia DR1 (Gaia Collaboration, 2016)
I/347 : Distances to 1.33 billion stars in Gaia DR2 (Bailer-Jones+, 2018)
J/MNRAS/415/103 : IPHAS T Tauri candidates in IC 1396 (Barentsen+, 2011)
J/A+A/537/A135 : X-ray view of IC348 (Stelzer+, 2012)
J/AJ/144/101 : Multiwavelength IRAS 20050+2720 young SFR (Guenther+, 2012)
J/MNRAS/426/91 : Kepler stars with infrared excess (Kennedy+, 2012)
J/MNRAS/426/2917 : X-rays sources in Trumpler 37 (Getman+, 2012)
J/A+A/559/A3 : Low-mass stars in Trumpler 37 (Sicilia-Aguilar+, 2013)
J/ApJS/208/9 : Intrinsic colors and temperatures of PMS stars (Pecaut+, 2013)
J/ApJ/787/109 : Age estimates for NGC 2024 and ONC stars (Getman+, 2014)
J/MNRAS/461/794 : Scorpius-Centaurus K-Type Stars (Pecaut+, 2016)
J/AJ/156/18 : APOGEE DR14:Binary comp. evolved stars (Price-Whelan+, 2018)
J/ApJ/868/43 : Adaptative optic images WISE YSO candidate (Silverberg+, 2018)
J/ApJ/878/7 : 2yr obs. of JHK variability of stars in Tr37 (Meng+, 2019)
Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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1- 14 I14 --- UKIRT UKIRT Source identifier
16- 41 A26 --- Spitzer Spitzer source identifier
43- 61 A19 --- WISE WISE source identifier
63- 73 F11.7 deg RAdeg [323/324] UKIRT Right Ascension (J2000)
75- 84 F10.7 deg DEdeg [57.2/57.8] UKIRT Declination (J2000)
86- 92 F7.4 mas plx [-0.008/2]? Gaia EDR3 parallax
94- 99 F6.4 mas e_plx [0.009/0.4]? Uncertainty in plx
101-106 F6.3 mag Jmag [10.3/21.7]? UKIRT/WFCAM J band Vega magnitude
108-112 F5.3 mag e_Jmag [0/0.2]? Uncertainty in Jmag
114-119 F6.3 mag Hmag [10/21.2]? UKIRT/WFCAM H band Vega magnitude
121-125 F5.3 mag e_Hmag [0/0.3]? Uncertainty in Hmag
127-132 F6.3 mag Kmag [9.47/19.5] UKIRT/WFCAM K band Vega magnitude
134-138 F5.3 mag e_Kmag [0/0.1] Uncertainty in Kmag
140-147 F8.2 uJy I1flux [16/97770]? Spitzer/IRAC I1 3.6um band flux
149-155 F7.4 uJy e_I1flux [0.4/28]? Uncertainty in I1flux
157-165 F9.3 uJy I2flux [8/61700]? Spitzer/IRAC I2 4.5um band flux
167-173 F7.4 uJy e_I2flux [0.3/23]? Uncertainty in I2flux
175-182 F8.2 uJy I3flux [53/74510]? Spitzer/IRAC I3 5.8um band flux
184-190 F7.3 uJy e_I3flux [1/261]? Uncertainty in I3flux
192-199 F8.2 uJy I4flux [25/87310]? Spitzer/IRAC I4 8.0um band flux
201-206 F6.3 uJy e_I4flux [1/82]? Uncertainty in I4flux
208-213 F6.3 mag W1mag [6.38/16.7]? WISE W1 3.368um band Vega magnitude
215-219 F5.3 mag e_W1mag [0.02/0.3]? Uncertainty in W1mag
221-226 F6.3 mag W2mag [6.33/17.5]? WISE W2 4.618um band Vega magnitude
228-232 F5.3 mag e_W2mag [0.01/0.5]? Uncertainty in W2mag
234-239 F6.3 --- alphaS [-2.51/1.91]? Spitzer-derived SED slope
241-246 F6.3 --- alphaW [-2.51/3.05]? WISE-derived SED slope
248-269 A22 --- Class Adopted YSO class
271-278 E8.2 mW/m2 xflux [1.3e-15/1.8e-13]? Combined (EPIC) X-ray flux;
0.2-12keV (1)
280-287 E8.2 mW/m2 e_xflux [1e-15/4e-14]? Uncertainty in xrayflux (1)
289-294 F6.3 --- HR [-1/0.98]? Hardness ratio (2)
296-300 F5.3 --- e_HR [0.02/1.1]? Uncertainty in HR
302-305 A4 --- Ref Previous references to source (3)
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Note (1): In units of erg/s/cm2.
Note (2): HR = (H-S)/(H+S) where "H" is 2-12keV band and "S" is 0.2-2keV band
Note (3): References as follows:
1 = Getman+, 2012, J/MNRAS/426/2917
2 = Barentsen+, 2011, J/MNRAS/415/103
3 = Sicilia-Aguilar+, 2005A&A...622A.118S 2005A&A...622A.118S
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History:
From electronic version of the journal
(End) Prepared by [AAS], Coralie Fix [CDS], 08-Mar-2022