J/ApJ/802/77 Protoplanetary disk masses in NGC 2024 cluster (Mann+, 2015)
Protoplanetary disk masses in the young NGC 2024 cluster.
Mann R.K., Andrews S.M., Eisner J.A., Williams J.P., Meyer M.R.,
Francesco J.D., Carpenter J.M., Johnstone D.
<Astrophys. J., 802, 77 (2015)>
=2015ApJ...802...77M 2015ApJ...802...77M
ADC_Keywords: Millimetric/submm sources ; YSOs
Keywords: circumstellar matter; protoplanetary disks; stars: formation;
stars: pre-main sequence
Abstract:
We present the results from a Submillimeter Array survey of the
887µm continuum emission from the protoplanetary disks around 95
young stars in the young cluster NGC 2024. Emission was detected from
22 infrared sources, with flux densities from ∼5 to 330mJy; upper
limits (at 3σ) for the other 73 sources range from 3 to 24mJy.
For standard assumptions, the corresponding disk masses range from
∼0.003 to 0.2M☉, with upper limits at 0.002-0.01M☉. The
NGC 2024 sample has a slightly more populated tail at the high end of
its disk mass distribution compared to other clusters, but without
more information on the nature of the sample hosts it remains unclear
if this difference is statistically significant or a superficial
selection effect. Unlike in the Orion Trapezium, there is no evidence
for a disk mass dependence on the (projected) separation from the
massive star IRS 2b in the NGC 2024 cluster. We suggest that this is
due to either the cluster youth or a comparatively weaker
photoionizing radiation field.
Description:
Observations at 887um of 9 distinct pointings containing a total of 95
young stars were conducted with the SMA in the fall of 2011, using the
compact array configuration (baselines of ∼8-50m).
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table2.dat 72 91 Inferred disk fluxes and masses from sub-millimer
array (SMA) observations
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See also:
J/MNRAS/435/1671 : SCUBA-2 850um survey in σOri cluster (Williams+, 2013)
J/ApJ/722/1092 : Optical photometry of the ONC. II. (Da Rio+, 2010)
J/ApJS/181/321 : Properties of Spitzer c2d dark clouds (Evans+, 2009)
J/ApJS/175/277 : Submillimeter-Continuum SCUBA detections (Di Francesco+, 2008)
J/ApJ/646/1215 : Low-mass stars and brown dwarfs in NGC 2024 (Levine+, 2006)
J/AJ/126/1916 : JHK photometry of young clusters near the Sun (Porras+, 2003)
J/AJ/126/1665 : NICMOS observations of NGC 2024 (Liu+, 2003)
J/ApJ/598/375 : Chandra X-ray observations of NGC 2024 (Skinner+, 2003)
J/ApJ/566/945 : Massive star forming regions at 1.2mm (Beuther+, 2002)
Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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1 A1 --- f_Fobs [n] non dectection (3σ upper limit are
given for Fobs)
3- 9 A7 --- Name Source designation (1)
11 I1 --- EC03 [1/9]? Source number in Eisner & Carpenter
(2003ApJ...598.1341E 2003ApJ...598.1341E); 3mm detection (2)
13 I1 --- IRS [2]? IRC 232 = IRS 2
15 A1 --- Fld [A-I] SMA field as in Figure 1 and Table 1
17- 18 I2 h RAh SMA emission centroid right ascension (J2000)
20- 21 I2 min RAm SMA emission centroid right ascension (J2000)
23- 26 F4.1 s RAs SMA emission centroid right ascension (J2000)
28 A1 --- DE- SMA emission centroid sign of declination (J2000)
29- 30 I2 deg DEd SMA emission centroid declination (J2000)
32- 33 I2 arcmin DEm SMA emission centroid declination (J2000)
35- 38 F4.1 arcsec DEs SMA emission centroid declination (J2000)
40- 44 F5.1 mJy Fobs [3/330.5] Integrated 887um continuum flux density
corrected for SMA primary beam attenuation
46- 48 F3.1 mJy e_Fobs [1/4.5]? Fobs uncertainty
50- 53 F4.1 mJy Fff [0.1/12]? Extrapolated contribution of free-free
emission at 887um (3)
55- 57 F3.1 mJy Fcld [0/0.9] Estimated contribution from large-scale
cloud emission
59- 63 F5.1 mJy Fdk [2.8/330.1] Derived dust continuum flux density
from the disk
65- 68 F4.1 cMsun Mdk [0.2/17.7] Inferred disk mass (in 0.01M☉)
70- 72 F3.1 cMsun e_Mdk [0.1/0.4]? Mdk uncertainty (4)
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Note (1): source designation, according to Meyer M.R., 1996, PhD thesis
Max-Planck-Institut fur Astronomie
Note (2): In two cases, IRC 106/098 and IRC 101/093, it is difficult to
unambiguously distinguish two potential associations with infrared
sources. See section 3.
Note (3): estimated from Rodriguez et al. (2003ApJ...598.1100R 2003ApJ...598.1100R) measurements
Note (4): Uncertainty does not include systematics in the absolute flux scale,
which contribute an additional ∼10%.
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History:
From electronic version of the journal
(End) Emmanuelle Perret [CDS] 23-Jul-2015