J/A+A/669/A22 Star formation in IC1396 (Pelayo-Baldarrago+, 2023)
Star formation in IC1396: Kinematics and subcluster structure revealed by Gaia.
Pelayo-Baldarrago M.E., Sicilia-Aguilar A., Fang M., Roccatagliata V.,
Kim J.S., Garcia-Alvarez D.
<Astron. Astrophys. 669, A22 (2023)>
=2023A&A...669A..22P 2023A&A...669A..22P (SIMBAD/NED BibCode)
ADC_Keywords: H II regions ; Stars, pre-main sequence ; Spectroscopy ;
Parallaxes, trigonometric ; Proper motions ; Optical
Keywords: globular clusters: individual: IC1396 - stars: formation -
stars: pre-main sequence - techniques: spectroscopic - HII regions -
ISM: jets and outflows
Abstract:
We investigate the star formation history of the IC1396 region by
studying its kinematics and completing the population census. We use
multiwavelength data, combining optical spectroscopy (to identify and
classify new members), near-infrared photometry (to trace shocks,
jets, and outflows and the interactions between the cluster members
and the cloud), along with Gaia EDR3 to identify new potential members
in the multidimensional proper motion/parallax space. The revised Gaia
EDR3 distance is 925±73pc, slightly closer than previously
obtained with DR2. The Gaia data reveal four distinct subclusters in
the region. These subclusters are consistent in distance but display
differences in proper motion. This, with their age differences, hints
towards a complex and varied star formation history. Gaia data also
unveil the intermediate-mass objects that tend to evade spectroscopic
and disk surveys. Our analysis allows us to identify 334 new members.
We estimate an average age of ∼4Myr, confirming previous age
estimates. With the new members added to our study, we estimate a disk
fraction of 28%, lower than previous values, due to our method
detecting mainly new, diskless intermediate-mass stars. We find age
differences between the subclusters, which evidences a complex star
formation history with different episodes of star formation.
Description:
Collection of IC1396 known members from literature plus Spectroscopy,
with their coordinates. Probabilities of the known members to belong
to each subcluster, resulting from the maximum likelihood analysis
from the Gaia EDR3 data, together with the astrometric parameters,
parallax, proper motions, RUWE. Astrometric parameters and
probabilities of the new members obtained from the Mahalanobis
distance analysis.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tablea1.dat 69 1538 Total collection of known members from the
literature
tabled1.dat 134 578 Subcluster probabilities for known members
tablee1.dat 108 334 New members found from the Mahalanobis distance
analysis, using the Gaia EDR3
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See also:
I/350 : Gaia EDR3 (Gaia Collaboration, 2020)
Byte-by-byte Description of file: tablea1.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 19 I19 --- GaiaEDR3 ?=- Gaia EDR3 number identifier
21- 30 F10.6 deg RAdeg Right Ascension (ICRS) at Ep=2016.0 (1)
32- 40 F9.6 deg DEdeg Declination (ICRS) at Ep=2016.0 (1)
42- 69 A28 --- Ref References (bibcode)
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Note (1): Coordinates are from Gaia EDR3, except for objects without Gaia
counterparts, for which we list the coordinates of the corresponding reference.
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Byte-by-byte Description of file: tabled1.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 19 I19 --- GaiaEDR3 Gaia EDR3 number identifier
21- 30 F10.6 deg RAdeg Right Ascension (ICRS) at Ep=2016.0
32- 40 F9.6 deg DEdeg Declination (ICRS) at Ep=2016.0
42- 46 F5.3 mas plx Parallax
48- 52 F5.3 mas e_plx Uncertainty in plx
54- 60 F7.3 mas/yr pmRA Proper motion in Right Ascension
62- 66 F5.3 mas/yr e_pmRA Uncertainty in pmRA
68- 74 F7.3 mas/yr pmDE Proper motion in Declination
76- 80 F5.3 mas/yr e_pmDE Uncertainty in pmDE
82- 86 F5.3 --- RUWE The Re-normalized Unit Weight Error (1)
88- 91 F4.2 % PA [0/1] Probability of a source to belong
to A subcluster (2)
93- 96 F4.2 % PB [0/1] Probability of a source to belong
to B subcluster (2)
98-101 F4.2 % PC [0/1] Probability of a source to belong
to C subcluster (2)
103-106 F4.2 % PD [0/1] Probability of a source to belong
to D subcluster (2)
108-111 F4.2 % PE [0/1] Probability of a source to belong
to E subcluster (2)
113-116 F4.2 % PF [0/1] Probability of a source to belong
to F subcluster (2)
118-121 F4.2 % PG [0/1] Probability of a source to belong
to G subcluster (2)
123-125 A3 --- Subcluster Subcluster to which the source belongs
127-128 A2 --- Memb Membership (3)
131-134 A4 --- Refs References of previous studies (4)
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Note (1): The RUWE is a statistical indicator obtained from the Unit Weight
Error (UWE) or astrometric chi-square that requires a renormalization
depending on the magnitude and color of the source.
Note (2): show the probability for each source belonging to one of the
subclusters, A, B, C, D, E, F, and the extended population G.
Note (3): Membership as follows:
Y = member, with probability >80%
P = probable member to belong to one of the subclusters, with probability <80%
P2 = probable member of belonging to two subclusters with probabilities >40%
NS = no subcluster, low probability of not belonging to any cluster
Note (4): References of previous studies as follows:
1 = 2004AJ....128..805S 2004AJ....128..805S, Sicilia-Aaguilar et al., Cat. J/AJ/128/805
2 = 2005AJ....130..188S 2005AJ....130..188S, Sicilia-Aaguilar et al., Cat. J/AJ/130/188
3 = 2006ApJ...638..897S 2006ApJ...638..897S, Sicilia-Aaguilar et al., Cat. J/ApJ/638/897
4 = 2009AJ....138....7M 2009AJ....138....7M, Mercer et al.
5 = 2009ApJ...702.1507M 2009ApJ...702.1507M, Morales-Calderon et al., Cat. J/ApJ/702/1507
6 = 2011MNRAS.415..103B 2011MNRAS.415..103B, Barentsen et al., Cat. J/MNRAS/415/103
7 = 2012MNRAS.426.2917G 2012MNRAS.426.2917G, Getman et al., Cat. J/MNRAS/426/2917
8 = 2012AJ....143...61N 2012AJ....143...61N, Nakano et al., Cat. J/AJ/143/61
9 = 2013AJ....145...15R 2013AJ....145...15R, Rebull et al., Cat. J/AJ/145/15
10 = 2013A&A...559A...3S 2013A&A...559A...3S, Sicilia-Aaguilar et al., Cat. J/A+A/559/A3
11 = 2015A&A...573A..19S 2015A&A...573A..19S, Sicilia-Aaguilar et al., Cat. J/A+A/573/A19
12 = 2019ApJ...878....7M 2019ApJ...878....7M, Meng et al., Cat. J/ApJ/878/7
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Byte-by-byte Description of file: tablee1.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 19 I19 --- GaiaEDR3 Gaia EDR3 number identifier
21- 30 F10.6 deg RAdeg Right Ascension (ICRS) at Ep=2016.0
32- 40 F9.6 deg DEdeg Declination (ICRS) at Ep=2016.0
42- 46 F5.3 mas plx Parallax
48- 52 F5.3 mas e_plx Uncertainty in plx
54- 59 F6.3 mas/yr pmRA Proper motion in Right Ascension
61- 65 F5.3 mas/yr e_pmRA Uncertainty in pmRA
67- 72 F6.3 mas/yr pmDE Proper motion in Declination
74- 78 F5.3 mas/yr e_pmDE Uncertainty in pmDE
80- 84 F5.3 --- RUWE The Re-normalized Unit Weight Error (1)
86- 89 F4.2 % PA ?=- Probability of a source to belong
to A subcluster (2)
91- 94 F4.2 % PB ?=- Probability of a source to belong
to B subcluster (2)
96- 99 F4.2 % PE ?=- Probability of a source to belong
to E subcluster (2)
101-104 F4.2 % PF ?=- Probability of a source to belong
to F subcluster (2)
106-108 A3 --- Subcluster Subcluster to which the source belongs
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Note (1): The RUWE is a statistical indicator obtained from the Unit Weight
Error (UWE) or astrometric chi-square that requires a renormalization depending
on the magnitude and color of the source.
Note (2): show the probability for each source belonging to one of the
subclusters, or in some cases, to two subclusters.
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Acknowledgements:
Mara Pelayo Baldarrago,, maraelizabeth.pelayo(at)estudiante.uam.es
(End) Patricia Vannier [CDS] 28-Oct-2022