J/ApJS/256/30 ALMA 1.33mm images of 10 FU Orionis-type stars (Kospal+, 2021)
Massive compact disks around FU Orionis-type young eruptive stars revealed by
ALMA.
Kospal A., Cruz-Saenz de Miera F., White J.A., Abraham P., Chen L.,
Csengeri T., Dong R., Dunham M.M., Feher O., Green J.D., Hashimoto J.,
Henning T., Hogerheijde M., Kudo T., Liu H.B., Takami M., Vorobyov E.I.
<Astrophys. J. Suppl. Ser., 256, 30-30 (2021)>
=2021ApJS..256...30K 2021ApJS..256...30K (SIMBAD/NED BibCode)
ADC_Keywords: Stars, pre-main sequence; Carbon monoxide; Radio continuum;
Millimetric/submm sources; Interferometry
Keywords: Young stellar objects; FU Orionis stars; Circumstellar disks
Submillimeter astronomy; Interferometry
Abstract:
The FU Orionis-type objects (FUors) are low-mass pre-main-sequence
stars undergoing a temporary but significant increase of mass
accretion rate from the circumstellar disk onto the protostar. It is
not yet clear what triggers the accretion bursts and whether the disks
of FUors are in any way different from the disks of nonbursting young
stellar objects. Motivated by this, we conducted a 1.3mm continuum
survey of 10 FUors and FUor-like objects with ALMA, using both the 7m
array and the 12m array in two different configurations to recover
emission at the widest possible range of spatial scales. We detected
all targeted sources and several nearby objects as well. To constrain
the disk structure, we fit the data with models of increasing
complexity from 2D Gaussian to radiative transfer, enabling comparison
with other samples modeled in a similar way. The radiative transfer
modeling gives disk masses that are significantly larger than what is
obtained from the measured millimeter fluxes assuming optically thin
emission, suggesting that the FUor disks are optically thick at this
wavelength. In comparison with samples of regular class II and class I
objects, the disks of FUors are typically a factor of 2.9-4.4 more
massive and a factor of 1.5-4.7 smaller in size. A significant
fraction of them (65%-70%) may be gravitationally unstable.
Description:
We observed our FU Orionis-type (FUor) targets with ALMA in Band 6
between 2016 October 9 and 2018 April 5. A detailed log of
observations can be found in Table 1.
For each object, we took observations with the 7m array and two
different configurations of the 12m array (TM2 being the more compact
C40-3 configuration and TM1 being the more extended C40-6
configuration). We used a standard frequency setup that covered the
J=2-1 line of 12CO, 13CO, and C18O in 0.58GHz wide spectral
windows.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 101 35 Log of our ALMA continuum observations
img/* . 10 *Individual ALMA images of the FU Orionis-type
(FUor) targets in FITS format
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Note on img/* : The FITS files in this archive were used to create Figure 1.
The files contain the CLEAN image of our targets, showing the inner
8"x8" region centered at the position of the target. All images were
created using uniform weighting to maximize the angular resolution.
The pixel size was chosen so that each beam is represented by 10 pixels.
The images in this archive have NOT been primary beam corrected.
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See also:
I/347 : Distances to 1.33 billion stars in Gaia DR2 (Bailer-Jones+, 2018)
J/AJ/145/94 : Luminosities of protostars from Spitzer (Dunham+, 2013)
J/AJ/147/140 : SED of 24 class I & class II FU Orionis stars (Gramajo+, 2014)
J/A+A/582/L12 : V960 Mon light curves (Hackstein+, 2015)
J/ApJ/828/46 : ALMA survey of Lupus protoplanetary disks. I. (Ansdell+, 2016)
J/AJ/153/240 : Protoplanetary disks in sigma Ori with ALMA (Ansdell+, 2017)
J/A+A/600/A141 : Orion A integral shaped filament image (Kainulainen+, 2017)
J/A+A/607/A39 : 7 FU Orionis-type stars CO spectral cubes (Feher+, 2017)
J/A+A/618/A79 : FU Orionis small-amplitude light variations (Siwak+, 2018)
J/ApJ/878/111 : Members in Serpens with Gaia DR2 (Herczeg+, 2019)
J/ApJ/890/130 : VANDAM survey of Orion protostars. II. (Tobin+, 2020)
J/A+A/646/A102 : FU Ori multi-band interferometric observations (Labdon+, 2021)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 11 A11 --- Name Name of the star
13- 16 I4 pc Dist [140/1574] Distance
18- 20 I3 pc e_Dist [10/350]? Negative uncertainty on Dist
22- 24 I3 pc E_Dist [10/600]? Positive uncertainty on Dist
26- 27 I2 h RAh Hour of right ascension (J2000)
29- 30 I2 min RAm Minute of right ascension (J2000)
32- 36 F5.2 s RAs Second of right ascension (J2000)
38 A1 --- DE- Sign of declination (J2000)
39- 40 I2 deg DEd Degree of declination (J2000)
42- 43 I2 arcmin DEm Arcminute of declination (J2000)
45- 48 F4.1 arcsec DEs Arcsecond of declination (J2000)
50- 60 A11 "Y:M:D" Date Date of observation (UT)
62- 64 A3 --- Conf Configuration
66- 69 F4.2 arcsec Res [0.1/5.2] Angular resolution
71- 74 F4.1 min Exp [3.1/22.8] Exposure time
76- 78 F3.1 mm PWV [0.2/2.3]? ALMA precipitable water vapour
80- 81 I2 m Baseline1 Lower range of baseline
82 A1 --- --- [-]
83- 86 I4 m Baseline2 Upper range of baseline
88-101 A14 --- FileName Name of the FITS file in subdirectory "img"
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History:
From electronic version of the journal
(End) Emmanuelle Perret [CDS] 31-Jan-2022