J/MNRAS/471/100 Hi-GAL compact source catalog. -71.0<l<67.0 (Elia+, 2017)
The Hi-GAL compact source catalogue.
I. The physical properties of the clumps in the inner Galaxy
(-71.0° < l < 67.0°).
Elia D., Molinari S., Schisano E., Pestalozzi M., Pezzuto S., Merello M.,
Noriega-Crespo A., Moore T.J.T., Russeil D., Mottram J.C., Paladini R.,
Strafella F., Benedettini M., Bernard J.P., Di Giorgio A., Eden D.J.,
Fukui Y., Plume R., Bally J., Martin P.G., Ragan S.E., Jaffa S.E.,
Motte F., Olmi L., Schneider N., Testi L., Wyrowski F., Zavagno A.,
Calzoletti L., Faustini F., Natoli P., Palmeirim P., Piacentini F.,
Piazzo L., Pilbratt G.L., Polychroni D., Baldeschi A., Beltran M.T.,
Billot N., Cambresy L., Cesaroni R., Garcia-Lario P., Hoare M.G., Huang M.,
Joncas G., Liu S.J., Maiolo B.M.T., Marsh K.A., Maruccia Y., Mege P.,
Peretto N., Rygl K.L.J., Schilke P., Thompson M.A., Traficante A.,
Umana G., Veneziani M., Ward-Thompson D., Whitworth A.P., Arab H.,
Bandieramonte M., Becciani U., Brescia M., Buemi C., Bufano F., Butora R.,
Cavuoti S., Costa A., Fiorellino E., Hajnal A., Hayakawa T., Kacsuk P.,
Leto P., Li Causi G., Marchili N., Martinavarro-Armengol S., Mercurio A.,
Molinaro M., Riccio G., Sano H., Sciacca E., Tachihara K., Torii K.,
Trigilio C., Vitello F., Yamamoto H.
<Mon. Not. R. Astron. Soc., 471, 100-143 (2017)>
=2017MNRAS.471..100E 2017MNRAS.471..100E (SIMBAD/NED BibCode)
ADC_Keywords: Surveys ; Milky Way ; Infrared sources
Keywords: catalogues - ISM: clouds - dust, extinction -
local interstellar matter - infrared: ISM - submillimetre: ISM
Abstract:
Hi-GAL (Herschel InfraRed Galactic Plane Survey) is a large-scale
survey of the Galactic plane, performed with Herschelin five infrared
continuum bands between 70 and 500µm. We present a band-merged
catalogue of spatially matched sources and their properties derived
from fits to the spectral energy distributions (SEDs) and heliocentric
distances, based on the photometric catalogues presented in Molinari
et al., covering the portion of Galactic plane -71.0°<l<67.0°.
The band-merged catalogue contains 100 922 sources with a regular SED,
24584 of which show a 70-µm counterpart and are thus considered
protostellar, while the remainder are considered starless. Thanks to
this huge number of sources, we are able to carry out a preliminary
analysis of early stages of star formation, identifying the conditions
that characterize different evolutionary phases on a statistically
significant basis. We calculate surface densities to investigate the
gravitational stability of clumps and their potential to form massive
stars. We also explore evolutionary status metrics such as the dust
temperature, luminosity and bolometric temperature, finding that these
are higher in protostellar sources compared to pre-stellar ones. The
surface density of sources follows an increasing trend as they evolve
from pre-stellar to protostellar, but then it is found to decrease
again in the majority of the most evolved clumps. Finally, we study
the physical parameters of sources with respect to Galactic longitude
and the association with spiral arms, finding only minor or no
differences between the average evolutionary status of sources in the
fourth and first Galactic quadrants, or between 'on-arm' and
'interarm' positions.
Description:
We presented the physical catalogue of Hi-GAL compact sources
extracted in the inner Galaxy (in the longitude range l=-71° to
67°).
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
hcatalog.dat 732 62438 High reliability Hi-GAL catalog
lcatalog.dat 732 38484 Low reliability Hi-GAL catalog
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See also:
J/ApJS/208/14 : BGPS. IX. Data release 2. (Ginsburg+, 2013)
J/A+A/565/A75 : ATLASGAL dust condensations in Galactic plane (Csengeri+ 2014)
J/AJ/149/64 : MIPSGAL 24µm point source catalog (Gutermuth+, 2015)
J/A+A/591/A149 : Hi-GAL. inner Milky Way: +68≥l≥70 (Molinari+, 2016)
Byte-by-byte Description of file: hcatalog.dat lcatalog.dat
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Bytes Format Units Label Explanations
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1- 6 I6 --- ID Running number (1)
8- 29 A22 --- Name Designation (HIGALBMGLLL.llll+B.bbbb) (2)
31- 40 F10.6 deg GLON Galactic longitude
42- 50 F9.6 deg GLAT Galactic latitude
52- 61 F10.6 deg RAdeg Right ascension (J2000)
63- 72 F10.6 deg DEdeg Declination (J2000)
74- 95 A22 --- Name70 Designation of the PACS 70-um counterpart (3)
97-104 F8.3 Jy F70 ?=0 Flux density at 70um of PACS 70um
counterpart
106-112 F7.3 Jy e_F70 ? rms uncertainty on F70
114-122 F9.3 Jy F70tot ?=0 Sum of fluxes of all PACS 70um
counterparts (4)
124-131 F8.3 Jy e_F70tot rms uncertainty on F70tot
133-139 F7.3 Jy F70add ?=0 Flux of the closest PACS 70um
counterpart (5)
141-146 F6.3 Jy e_F70add rms uncertainty on F70add
148-154 F7.3 Jy F70addtot ?=0 Sum of fluxes of all PACS 70um
counterparts (6)
156-161 F6.3 Jy e_F70addtot rms uncertainty on F70addtot
163-169 F7.3 Jy F70lim ?=0 5σ upper limit in the PACS 70-um
band, estimated where
both F70tot=0 and F70addtot=0
171-192 A22 --- Name160 Designation of the PACS 160-um counterpart (3)
194-201 F8.3 Jy F160 ?=0 Flux density at 160um of PACS 160um
counterpart
203-209 F7.3 Jy e_F160 ? rms uncertainty on F160
211-218 F8.3 Jy F160add ?=0 Sum of fluxes of all PACS 160um
counterparts (4)
220-226 F7.3 Jy e_F160add rms uncertainty on F160add
228-234 F7.3 Jy F160lim ?=0 5σ upper limit in the PACS 70-um
band, estimated where
both F160tot=0 and F160addtot=0
236-257 A22 --- Name250 Designation of the SPIRE 250um counterpart (3)
259-266 F8.3 Jy F250 ?=0 Flux density at 250um of SPIRE 250um
counterpart
268-275 F8.3 Jy e_F250 ? rms uncertainty on F250
277-298 A22 --- Name350 Designation of the SPIRE 350um counterpart (3)
300-307 F8.3 Jy F350 ?=0 Flux density at 350um of SPIRE 350um
counterpart
309-316 F8.3 Jy e_F350 ? rms uncertainty on F350
318-325 F8.3 Jy F350FSC ?=0 SPIRE 350um flux scaled, as mentioned
in Section 3.1
327-333 F7.3 Jy e_F350FSC ?=0 rms uncertainty on F350FSC
335-356 A22 --- Name500 Designation of the SPIRE 500um counterpart (3)
358-365 F8.3 Jy F500 ?=0 Flux density at 500um of SPIRE 500um
counterpart
367-373 F7.3 Jy e_F500 ? rms uncertainty on F500
375-382 F8.3 Jy F500FSC ?=0 SPIRE 500um flux scaled, as mentioned
in Section 3.1
384-390 F7.3 Jy e_F500FSC rms uncertainty on F500FSC
392-414 A23 --- Name21 Designation of the MSX 21-um counterpart, as
defined in the MSX point source catalogue
416-423 F8.3 Jy F21 ?=0 Flux at 21um of the closest MXS 21um
counterpart
425-431 F7.3 Jy e_F21 ?=0 rms uncertainty on F21
433-440 F8.3 Jy F21tot ?=0 Sum of fluxes of all MXS 21um
counterparts (7)
442-448 F7.3 Jy e_F21tot ?=0 rms uncertainty on F21tot
450-468 A19 --- Name22 Designation of the WISE 22um counterpart
470-477 F8.3 Jy F22 ?=0 Flux at 22um of the closest WISE 22um
counterpart
479-483 F5.3 Jy e_F22 ?=0 rms uncertainty on F22
485-492 F8.3 Jy F22tot ?=0 Sum of fluxes of all WISE 22um
counterparts (7)
494-498 F5.3 Jy e_F22tot ?=0 rms uncertainty on F22tot
500-517 A18 --- Name24 Designation of the MSX 24um counterpart (8)
519-526 F8.3 Jy F24 ?=0 Flux at 24um of the closest
MIPSGAL 24um counterpart
528-532 F5.3 Jy e_F24 ?=0 rms uncertainty on F24
534-539 F6.3 Jy F24tot ?=0 Sum of fluxes of all MIPSGAL 24um
counterparts (7)
541-545 F5.3 Jy e_F24tot ?=0 rms uncertainty on F24tot
547-562 A16 --- Name870 Designation of the ATLASGAL 870um
counterpart (9)
564-570 F7.3 Jy F870 ?=0 Flux at 870um of the closest
ATLASGAL 870um counterpart
572-577 F6.3 Jy e_F870 ?=0 rms uncertainty on F870
579-600 A22 --- Name1100 Designation of the BGPS 1100um
counterpart (10)
602-607 F6.3 Jy F1100 ?=0 Flux at 1100um of BOLOCAM 1100um
counterpart
609-613 F5.3 Jy e_F1100 ?=0 rms uncertainty on F1100
615-619 F5.2 arcsec DFWHM250 Circularized and (if the circularized size
exceeds the instrumental beam size by a
factor of psrt(2) beam-deconvolved size of
the sources as estimated by CuTEx in
the 250-um band
621-625 I5 pc Dist ?=0 Kinematic distance of the source (11)
627-632 I6 pc NearDist ?=0 Near distance (11)
634-638 I5 pc FarDist ?=0 Far distance (11)
640 A1 --- f_Dist [BG-] Flag indicating the quality of the
distance near/far ambiguity solution (12)
642-646 F5.3 pc Diam Source linear diameter, in pc, obtained by
combining DFWHM250 and Dist
648-654 F7.2 Msun MLars ?=0 Larson's mass
656-657 A2 --- FitType [Tk Tn] Flag on SED (13)
659 I1 --- Fevol [0/2] Flag indicating the evolutionary
classification of the source (14)
661 A1 --- n_Mass [-] "-" for Mass calculated with a virtual
distance of 1kpc (15)
662-670 F9.2 Msun Mass Clump total mass (15)
672-679 F8.2 Msun e_Mass [] rms uncertainty on Mass
681-685 F5.2 K Tdust Dust temperature of the clump, derived from
the grey-body fit
687-690 F4.2 K e_Tdust rms uncertainty on Tdust
692-696 F5.1 um lambda0 ?=0 Value of λ0, derived from the
grey-body fit
698 A1 --- n_Lbol [-] "-" for Lbol calculated with a virtual
distance of 1kpc (16)
699-708 F10.2 Lsun Lbol Bolometric luminosity (16)
710-718 F9.2 --- Lratio ? Ratio between the bolometric luminosity and
its fraction computed over the range
λ≥350um
719 A1 --- n_Lratio [I] I for infinity
720-725 F6.2 K Tbol Bolometric temperature, calculated based on
equation (5) of the paper
727-732 F6.3 g/cm2 SurDens Surface density (17)
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Note (1): starting from 1 in the high-reliability table and continuing in
the low-reliability one.
Note (2): string composed by 'HIGAL', 'BM' (which stays for 'band-merged') and
Galactic coordinates of the sources, chosen as the coordinates of the
shortest wavelength available Hi-GAL counterpart.
Note (3): as defined in the catalogue of Molinari et al.
(2016, Cat. J/A+A/591/A149).
Note (4): sum of fluxes of all PACS 70um counterparts (if available) lying
inside the half-maximum ellipse of the source detected by CuTEx in the
SPIRE 250-um maps. By definition, F70tot≥F70. The null value is 0.
This is the flux at 70um actually used to estimate the source bolometric
luminosity and temperature).
Note (5): Flux of the closest PACS 70-um counterpart (if available) found
through targeted source extraction at a detection threshold lower than in
Molinari et al. (2016, Cat. J/A+A/591/A149) where F70tot=0.
Note (6): Sum of fluxes of all PACS 70-um counterparts (if available) found
through targeted source extraction at a detection threshold lower than in
Molinari et al. (2016, Cat. J/A+A/591/A149), where F70tot=0, and lying inside
the ellipse at 250um (as for F70tot). This is the flux at 70um
actually used to estimate the source bolometric luminosity and temperature
where F70tot=0.
Note (7): lying inside the ellipse at 250um (as done for F70tot)
Note (8): A string beginning with 'MG' identifies a source taken from the
catalogue of Gutermuth & Heyer (2015, Cat. J/AJ/149/64), while a string
beginning with 'D' identifies a source specifically detected in this work,
(cf. Section 3.3). Furthermore, a lack of a source due to saturation is
identified with the 'saturated' string.
Note (9): A string beginning with 'G' identifies a source taken from the
catalogue of Csengeri et al. (2014, Cat. J/A+A/565/A75), while the string
'CuTEx' identifies a source specifically detected for this work, as explained
in Section 3.3.
Note (10): as defined in the BGPS catalogue (Ginsburg et al., 2013,
Cat. J/ApJS/208/14).
Note (11): using method described in Russeil et al., 2011A&A...526A.151R 2011A&A...526A.151R.
Note (12): Flag indicating the quality of the distance near/far ambiguity
solution as follows:
G = an external indicator is used to take the decision
B = far distance is assigned to the source by default (see Section 3.4)
Note (13): Flag as follows:
Tk = thick case, expression of the grey body fitted to the source SED
is given by equation (1)
Tn = thin case, expression of the grey body fitted to the source SED
is given by equation (4)
Note (14): flag as follows:
0 = starless unbound
1 = prestellar
2 = protostellar
Note (15): Clump total mass, derived by fitting a grey body to the source SED.
In the case of an unavailable distance, the fit is performed anyway assuming a
virtual distance of 1 kpc, and f_Mass="-" (original Mass value quoted as
a negative value).
Note (16): For sources devoid of a distance estimate, a luminosity corresponding
to the virtual distance of 1kpc is calculated and f_Lbol="-"
(original Lbol quoted as a negative value).
Note (17): Surface density, calculated by dividing the mass (Mass) by the area
of the circle with the diameter (Diam). Where the distance is unavailable,
this quantity can be evaluated anyway, assuming a whatever virtual distance
for intermediate calculations, and starting from DFWHM250 instead of Diam.
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History:
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(End) Patricia Vannier [CDS] 14-May-2020