J/ApJ/799/100 Herschel FIR observations of NGC3603 (Di Cecco+, 2015)
Herschel far-IR observations of the giant H II region NGC 3603.
Di Cecco A., Faustini F., Paresce F., Correnti M., Calzoletti L.
<Astrophys. J., 799, 100 (2015)>
=2015ApJ...799..100D 2015ApJ...799..100D
ADC_Keywords: Clusters, open ; Photometry, infrared ; H II regions ; YSOs
Keywords: open clusters and associations: individual: NGC 3603;
stars: pre-main sequence
Abstract:
We observed the giant H II region around the NGC 3603 young stellar
cluster (YC) with the five broad bands (70, 160, 250, 350, 500µm)
of the SPIRE and PACS instruments, on board the Herschel Space
Observatory. Together with what is currently known of the stellar,
atomic, molecular, and warm dust components, this additional and
crucial information should allow us to better understand the details
of the star-formation history in this region. The main objective of
the investigation is to study, at high spatial resolution, the
distribution and main physical characteristics of the cold dust. By
reconstructing the temperature and density maps, we found,
respectively, a mean value of 36K and log10NH=22.0±0.1/cm2. We
carried out a photometric analysis detecting 107 point-like sources,
mostly confined to the north and south of the cluster. By comparing
our data with spectral energy distribution models, we found that 35
sources are well represented by young stellar objects in early
evolutionary phases, from Class 0 to Class I. The Herschel detections
also provided far-IR counterparts for 4 H2O masers and 11 objects
previously known from mid-IR observations. The existence of so many
embedded sources confirms the hypothesis of intense and ongoing
star-formation activity in the region around NGC 3603 YC.
Description:
The cloud complex surrounding NGC 3603 YC was observed by Herschel
SPIRE/PACS during the Hi-GAL Survey (Molinari et al.
2010A&A...518L.100M 2010A&A...518L.100M, 2010PASP..122..314M 2010PASP..122..314M), a Key Programme that mapped
the Galactic plane in five photometric bands (70, 160, 250, 350, and
500um).
The MSX (Egan et al. 2003AAS...203.5708E 2003AAS...203.5708E) images were taken at
(wavelengths) 8.3, 12.1, 14.7, and 21.3um using the scan observing
mode, and the WISE (Wright et al. 2010AJ....140.1868W 2010AJ....140.1868W) images were
acquired in freeze-frame scan mode at 3.4, 4.6, 12, and 22um.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table2.dat 115 107 *Sources detected by Herschel in the Nurnberger
et al. N02 region (2002A&A...394..253N 2002A&A...394..253N), and
their MSX counterparts
table3.dat 81 35 SED analysis physical parameters
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Note on table2.dat: The WISE measurements are only for the detections in
common between Herschel and MSX.
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See also:
VI/139 : Herschel Observation Log (Herschel Science Centre, 2013)
II/311 : WISE All-Sky Data Release (Cutri+ 2012)
V/114 : MSX6C Infrared Point Source Catalog (Egan+ 2003)
J/ApJ/719/1104 : Massive star forming complexes in GLIMPSE (Rahman+, 2010)
J/A+A/481/345 : SED evolution in massive YSOs (Molinari+, 2008)
J/ApJ/675/1319 : Infrared photometry of NGC 3603 (Harayama+, 2008)
J/MNRAS/368/253 : Emission lines in M16, M20, NGC 3603 (Garcia-Rojas+, 2006)
J/AJ/127/1014 : CCD UBVRIHa photometry in NGC 3603 (Sung+, 2004)
J/MNRAS/327/23 : CCD UBVRI photometry of 7 open star clusters (Sagar+, 2001)
J/A+A/291/943 : Protostellar cores (Ossenkopf+, 1994)
http://www.asdc.asi.it/mmia/index.php?mission=herschel : ASDC Herschel archive
Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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1- 3 I3 --- Seq [1/107] Running sequence number
5- 8 A4 --- n_Seq Note on fit (1)
10- 11 I2 h RAh Hour of right ascension (J2000)
13- 14 I2 min RAm Minute of right ascension (J2000)
16- 20 F5.2 s RAs Second of right ascension (J2000)
22 A1 --- DE- Sign of declination (J2000)
23- 24 I2 deg DEd Degree of declination (J2000)
26- 27 I2 arcmin DEm Arcminute of declination (J2000)
29- 33 F5.2 arcsec DEs Arcsecond of declination (J2000)
35- 38 F4.2 Jy S3.4 [0.01/0.2]? WISE 3.4um flux density
40- 43 F4.2 Jy S4.6 [0.02/1.1]? WISE 4.6um flux density
45- 48 F4.2 Jy S8.3 [0.03/4.5]? MSX 8.3um flux density
50 A1 --- l_S8.3 [U] Upper limit flux (calculated via Eq.(4))
52- 55 F4.2 Jy S12.1 [0.01/4.3]? MSX 12.1um flux density
57 A1 --- l_S12.1 [U] Upper limit flux (calculated via Eq.(4))
59- 62 F4.2 Jy S14.7 [0.01/7.4]? MSX 14.7um flux density
64 A1 --- l_S14.7 [U] Upper limit flux (calculated via Eq.(4))
66- 70 F5.2 Jy S21.3 [0.02/27.3]? MSX 21.3um flux density
72 A1 --- l_S21.3 [U] Upper limit flux (calculated via Eq.(4))
74- 80 F7.3 Jy S70 [14.3/667.1]? Herschel/PACS 70um flux density
82 A1 --- l_S70 [U] Upper limit flux (calculated via Eq.(4))
84- 90 F7.2 Jy S160 [4.8/1382.1]? Herschel/PACS 160um flux density
92 A1 --- l_S160 [U] Upper limit flux (calculated via Eq.(4))
94- 99 F6.2 Jy S250 [4.4/659.7]? Herschel/SPIRE 250um flux density
101 A1 --- l_S250 [U] Upper limit flux (calculated via Eq.(4))
103-108 F6.2 Jy S350 [2.4/425.7]? Herschel/SPIRE 350um flux density
110-115 F6.2 Jy S500 [4.3/197.9]? Herschel/SPIRE 500um flux density
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Note (1): Flag as follows:
d = source fitted with a SED model
B = Counterpart of B10 (Breen et al. 2010MNRAS.406.1487B 2010MNRAS.406.1487B) source
(see the B10 properties in table 4)
NS = Counterpart of NS03 (Nuernberger et al. 2003A&A...400..223N 2003A&A...400..223N) source.
(see the NS03 properties in table 4)
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Byte-by-byte Description of file: table3.dat
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Bytes Format Units Label Explanations
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1- 3 I3 --- Seq [1/106] Running sequence number as in table2
5- 9 F5.2 kLsun Lbol0 [1/48] Observed bolometric luminosity (2)
11- 15 F5.2 kLsun e_Lbol0 [0.4/17] Lbol0 uncertainty
17- 21 F5.2 kLsun LbolT [0.8/41] Theoretical bolometric luminosity (2)
23- 26 F4.2 kLsun e_LbolT [0.02/6.4] LbolT uncertainty
28- 31 F4.2 kMsun Menv [0.01/2.8] Envelope mass (in 103M☉)
33- 36 F4.2 kMsun e_Menv [0/0.5] Menv uncertainty
38- 41 F4.2 Msun/kyr dM/dt [0.2/6.2] Accretion rate (in 10-3M☉/yr)
43- 46 F4.2 Msun/kyr e_dM/dt [0.01/0.86] dM/dt uncertainty
48- 51 F4.1 Msun M* [7.8/27.2] Central stellar mass
53- 55 F3.1 Msun e_M* [0.1/1.7] M* uncertainty
57- 61 F5.2 kK T* [3.6/34.8] Stellar temperature
63- 66 F4.2 kK e_T* [0.03/1.4] T* uncertainty
68- 73 F6.2 kyr Age [0.9/131.8] Age
75- 79 F5.2 kyr e_Age [0.1/23.5] Age uncertainty
81 A1 --- Cl [0I] YSO class (0 or I)
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Note (2): Luminosities in 103L☉.
The observed bolometric luminosity Lbol0 is calculated for a
distance of 7Kpc, while the theoretical bolometric luminosity LbolT
and its uncertainty are calculated for a distance of 7±1Kpc.
See section 2.2.
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History:
From electronic version of the journal
(End) Emmanuelle Perret [CDS] 15-Jun-2015