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Table 1

Line fluxes for Cha II members observed with Herschel-PACS.

Name RA Dec Sp. type Class OBSID [OI] flux FWHM [ OI ] o-H2O flux FWHM H2O
@ 63.185 μm @63.324 μm
– – – – – – (10-17 W/m2) (μm) (10-17 W/m2) (μm)
DK Cha 12 53 17.23 –77 07 10.7 F0 I-II 1342226006 190.0 ± 0.7 * – < 2.9 –
384 ± 2 **
IRAS 12500-7658 12 53 42.86 –77 15 11.5 M6.5 I 1342226005 5.04 ± 0.25 0.021 < 0.55 –
Sz 46N 12 56 33.66 –76 45 45.3 M1 II 1342226009 < 0.75 – < 0.75 –
IRAS 12535-7623 12 57 11.77 –76 40 11.3 M0 II 1342226010 < 0.91 – < 0.91 –
ISO ChaII 13 12 58 06.78 –77 09 09.4 M7 II 1342228419 < 0.69 – < 0.69 –
Sz 50 13 00 55.36 –77 10 22.1 M3 II 1342226008 < 0.65 – < 0.65 –
Sz 51 † 13 01 58.94 –77 51 21.7 K8.5 II 1342229799 0.43 ± 0.14 0.012 < 0.68 –
[VCE2001] C50 13 02 22.85 –77 34 49.3 M5 II 1342227072 < 0.66 – < 0.66 –
Sz 52 13 04 24.92 –77 52 30.1 M2.5 II 1342229800 1.2 ± 0.3 0.024 < 0.73 –
Hn 25 13 05 08.53 –77 33 42.4 M2.5 II 1342227071 < 0.75 – < 0.75 –
Sz 53 13 05 12.69 –77 30 52.3 M1 II 1342229829 < 0.76 – < 0.76 –
Sz 54 13 05 20.68 –77 39 01.4 K5 II 1342229831 1.5 ± 0.4 0.032 < 0.74 –
J13052169-7738102 13 05 21.66 –77 38 10.0 – Flat 1342229830 0.81 ± 0.23 0.018 < 0.68 –
J13052904-7741401 13 05 29.04 –77 41 40.1 – II 1342229832 < 0.78 – < 0.78 –
[VCE2001] C62 13 07 18.05 –77 40 52.9 M4.5 II 1342229833 < 0.70 – < 0.70 –
Hn 26 * 13 07 48.51 –77 41 21.4 M2 II 1342228418 < 0.71 – < 0.71 –
Sz 61 13 08 06.28 –77 55 05.2 K5 II 1342229801 0.87 ± 0.22 0.028 0.56 ± 0.15 0.012
[VCE2001] C66 13 08 27.17 –77 43 23.2 M4.5 II 1342228419 < 0.72 – < 0.72 –
Sz 62 13 09 50.38 –77 57 23.9 M2.5 II 1342228420 < 0.63 – < 0.63 –

Notes. Spectral types taken from Spezzi et al. (2008). SED classes (after Lada 1987) from Alcalá et al. (2008). FWHMs are not corrected for instrumental resolution.

(*)

Line flux from integration of the observed central spaxel spectrum.

(**)

Line flux integration of the 5 × 5 co-added spectrum.

(†)

The FWHM of the Gaussian fit is slightly smaller than the instrumental value, therefore the upper limit, computed using instrumental FWHM, is larger than the detected flux.

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