2008A&A...482..855H


C.D.S. - SIMBAD4 rel 1.7 - 2020.10.24CEST16:59:55

2008A&A...482..855H - Astronomy and Astrophysics, volume 482, 855-863 (2008/5-2)

Star formation in Perseus. IV. Mass-dependent evolution of dense cores.

HATCHELL J. and FULLER G.A.

Abstract (from CDS):

In our SCUBA survey of Perseus, we find that the fraction of protostellar cores increases towards higher masses and the most massive cores are all protostellar. In this paper we consider the possible explanations of this apparent mass dependence in the evolutionary status of these cores. We investigate the implications for protostellar evolution and the mapping of the embedded core mass function (CMF) onto the stellar IMF. We consider the following potential origins of the observed behaviour: dust temperature, selection effects in the submillimetre and in the mid-infrared observations used for pre/protostellar classification, confusion and multiplicity, transient cores, and varying evolutionary timescales. We develop core mass evolution diagrams (CMEDs) to investigate how the mass evolution of individual cores maps onto the observed CMF. We find that two physical mechanisms - short timescales for the evolution of massive cores, and continuing accumulation of mass onto protostellar cores - best explain the relative excess of protostars in high mass cores and the rarity of massive starless cores. In addition, we show that confusion both increases the likelihood that a protostar is identified within a core, and increases mass assigned to a core. Selection effects and/or transient cores also contribute to an excess of starless cores at low masses. The observed pre/protostellar mass distributions are consistent with faster evolution and a shorter lifetime for higher-mass prestellar cores. The differences in the prestellar and protostellar mass distributions imply that the prestellar CMF (and possibly the combined pre+protostellar CMF) should be steeper than the IMF. A steeper prestellar CMF can be reconciled with the observed similarity of the CMF and the IMF in some regions if a second opposing effect is present, such as the fragmentation of massive cores into multiple systems.

Abstract Copyright:

Journal keyword(s): submillimeter - stars: formation - ISM: clouds

Simbad objects: 17

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Number of rows : 17

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 LDN 1448 DNe 03 22.5 +30 35           ~ 469 0
2 LDN 1448NW Y*O 03 25 35.66 +30 45 34.2           ~ 61 0
3 IRAS F03226+3033 Y*O 03 25 38.83 +30 44 06.2           ~ 304 0
4 [SDA2014] West4 Y*O 03 25 38.83 +30 44 06.2           ~ 242 1
5 [JCC87] IRAS 2A Y*O 03 28 55.55 +31 14 36.7           ~ 402 3
6 BD+30 547 Y*O 03 28 57.2107612240 +31 14 19.076624755   10.73 9.98 9.1   G4V 93 1
7 [JCC87] IRAS 4A Y*O 03 29 10.49 +31 13 30.8           ~ 608 1
8 [JCC87] IRAS 4 FIR 03 29 10.9 +31 13 26           ~ 468 0
9 NGC 1333 OpC 03 29 11 +31 18.6           ~ 1231 1
10 [JCC87] IRAS 4B Y*O 03 29 12.058 +31 13 02.05           ~ 562 0
11 Barnard 1 MoC 03 33 16.3 +31 07 51           ~ 266 0
12 [HKM99] B1-b cor 03 33 20.32 +31 07 21.5           ~ 164 0
13 HH 211 cor 03 43 56.52 +32 00 52.8           ~ 296 0
14 IC 348 OpC 03 44 34 +32 09.8           ~ 1236 1
15 NAME Ophiuchus Molecular Cloud SFR 16 28 06 -24 32.5           ~ 3066 0
16 NAME Serpens Cloud SFR 18 29 49 +01 14.8           ~ 927 2
17 NAME Cyg X Cld 20 28 41 +41 10.2           ~ 633 1

    Equat.    Gal    SGal    Ecl

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2020.10.24-16:59:55

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