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Table 1

3.6 μm coreshine intensity and 4.5/3.6 coreshine ratio sorted by increasing ratio value for each detected cloud of the four regions.

Name 3.6 μm intensity 4.5/3.6 Protostar Classa LBolb Refs.
kJy sr-1 median FWHM L⊙
Taurus-Perseus
G171.80−09.78 10 – –
CB24 15 – –
L1503 22 – –
G179.18−19.62 22 – –
G182.19−17.71 23 – –
G170.81−18.34 26 – –
L1552 26 – –
G169.82−19.39 27 – –
CB20 27 – –
G173.45−13.34 30 – –
G177.89−20.16 33 – –
B18–3 = G174.39−13.43 35 –
G154.68−15.34 49 0.35 0.10
G170.99−15.81 36 0.36 0.17
L1506C 33 0.37 0.26
L1507A (G171.51−10.59) 41 0.41 0.15
IRAS 03282+3035 47 0.42 0.14 IRAS 03282+3035 Class 0 1.2 1
G173.69−15.55 32 0.43 0.10
L1544 39 0.43 0.32
L1512 30 0.44 0.31
L1521E 51 0.46 0.25
L1498 34 0.47 0.22
G171.34−10.67 58 0.47 0.20
G170.26−16.02 87 0.50 0.30 IRAS 04181+2654AB Class I – 2
L1521F 53 0.51 0.20 VeLLOc Class 0 0.36 3
L1517A 57 0.51 0.28
L1517B 43 0.51 0.28
G157.10−08.70 34 0.52 0.15 IRAS 03586+4112 (?)d
L1517C 29 0.53 0.28
L1507 41 0.54 0.35 2MASS J04432023+2940060 Class II – 4
IRAM 04191 140 0.57 0.36 IRAM 04191–IRS Class 0 0.28 5
L1439 81 0.60 0.29 IRAS 04559+5200 Class I ≥0.5 6, 7
TMC2 e 100 0.64 0.47 IRAS 04294+2413 Class 0 ? 0.78 (LIR) 8
L1448mm 59 0.64 0.44 L1448-mm Class 0 8.6 9
G163.21−08.40 67 0.64 0.46 IRAS 04218+3708 (?)d
G157.12−11.56 390 0.64 0.39 IRAS 03484+3845 (?)d
G155.45−14.59 210 0.64 0.27 IRAS 03330+3727 (?)d
G160.51−16.84 61 0.66 0.51 B5 IRS1 (IRAS 03445+3242) Class I 3.8 10
G171.91−15.65 310 0.77 0.39 DG Tau B Class I 0.86 2, 11
Barnard18–1 97 0.79 0.39 IRAS 04292+2422(E+W) Class I 0.6 10
G163.32−08.42 63 0.82 0.30 IRAS 04223+3700 Class 1 2.7 10
G158.86−21.60 74 0.95 0.40 IRAS 03249+2957 Class I 0.3 1
Barnard1 100 1.1 0.51 IRAS 03301+3057 (cluster) Class I 2.7 (LIR) 12
L183/L134
L183 58 0.37 0.14
L134 f >30 – –
Chameleon
G302.89−14.05 16 – –
G298.34−13.03 25 – –
G303.28−13.32 25 – –
Mu8 27 – –
G297.09−16.02 39 0.35 0.23
G303.09−16.04 77 0.43 0.23
G303.68−15.32 21 0.44 0.23
G303.39−14.26 150 0.50 0.33 IRAS 12553−7651 Class I 1.2 13
G303.15−17.34 g 32 0.60 0.36
G303.72−14.86 100 0.74 0.52 IRAS 13014−7723 Class II 1.6 14, 15
Cepheus
G093.20+09.53 18 – –
L1155E 22 – –
G093.16+09.61 24 – –
G130.56+11.51 24 – –
L1157 28 0.41 0.09 IRAS 20386+6751 Class 0 11 16
L1155C 29 0.44 0.17
L1247 110 0.46 0.36
L1251A 62 0.50 0.40 L1251A–IRS1–4 Class I, I, 0 & 0 IRS3 = 0.8 17
L1333 h 25 0.50 0.18
L1148 24 0.54 0.38 L1148–IRS Class I 0.44 18
L1152 39 0.58 0.24 L1152 1–3 Class 0, I, & I 1.5, 0.6, 2.1 18
L1262 92 0.62 0.33 IRAS 23238+7401 Class 0 1.5 19
L1157–outflow 31 0.71 0.22 Outflow shock region ?
L1228 110 0.73 0.50 IRAS 20582+7724 (cluster) Class I 2.3 18
L1221 160 0.81 0.52 L1221–IRS1 & 3 Class 0 & 0 3.0 & 1.4 18
L1251C i 260 0.81 0.59 IRAS 22343+7501 (cluster) Class I 33 18
L1251B j 160 0.89 0.57 IRAS 22376+7455 (cluster) Class 0 15 18

Notes.

(a)

Protostar classes depend on the criterion (spectral index or TBol). Whenever possible, we used the second one. Geometry effects also count. See Robitaille et al. (2007) and Kirk et al. (2009) for further details.

(b)

If (LIR) is indicated, it is the integrated IR luminosity, because LBol is not available.

(c)

VEry Low-Luminosity Object.

(d)

A bright IRAS source is observed in the vicinity of the cloud, but no study of the source has been found in the literature. Its YSO status is therefore not proved but probable.

(e)

TMC2 is usually considered to be starless (e.g., Brady Ford & Shirley 2011). The IRAC coreshine images and ratio show that the nearby YSO at ~4′ is illuminating it.

(f)

The Spitzer L134 3.6 μm map is too narrow compared with the coreshine extent in the WISE image and a part of the flux is missing.

(g)

A bright star at position 12h57m20s −80°15′42′′ (J2000) seems to illuminate the cloud. It is not listed in SIMBAD.

(h)

L1333 contains a submm source: JCMTSF J022611.7+752732 (Di Francesco et al. 2008).

(i)

Kirk et al. (2009) have renamed L1251A as L1251W, and L1251C as L1251A. We kept the SIMBAD definition of the source parts.

(j)

This part of the L1251 source is named either L1251B or L1251E, depending on the authors; SIMBAD separates them by 3.5′.

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