Table 5
Sources in which HOOH has been searched for.
Source | HOOH | HOOH | Ref. |
---|---|---|---|
rms | ∫ Tmbdv | ||
(mK) | (mK km s−1) | ||
ρ Oph-A | 167 (a) | [1] | |
Orion “H2-Peak 1” | 26.1 (b) | 172 (b) | [2] |
r Oph-B2-MM8 | 22.9 | [3] | |
G15.01-0.67 | 19.2 | [3] | |
G018.82-00.28MM1 | 21.1 | [3] | |
G018.82-00.28MM4 | 21.0 | [3] | |
G028.53-00.25MM1 | 17.7 | [3] | |
NGC 6334I(N) | 18.6 | [3] | |
G1.6-0.025 | 16.1 | [3] | |
NGC 1333-IRAS 4A | 24.6 | [3] | |
L1527 | 18.4 | [3] | |
R CrA-IRS 7B | 23.1 | [3] | |
IRAS 16293-2422 | <67 | [4] | |
R CrA-IRS 5A | 9.7(a) | ≤10.2(a) | [5] |
NGC 1333-IRAS 2A | 8.0(a) | ≤13.5(a) | [5] |
L1551-IRS 5 | 2.1(c) | ≤4.3(c) | [5] |
L1544 | 5.0(c) | ≤4.5(c),(d) | [5] |
Notes. (a) Transition 30,3 − 21,1 at 219.167 GHz; (b)value from transition 30,3−21,1 at 219.167 GHz, which is one of five observed HOOH transitions, with the best S/N. Here the integrated area is given in ∫ TAdv and not in ∫ Tmbdv; (c) value from transition 41,3 − 30,3 at 143.712 GHz; (d)instead of using the mean FWHM value in Table 3, we assumed the higher FWHM value to estimate the upper limit.
References. [1] Bergman et al. (2011a), [2] Liseau & Larsson (2015), [3] Parise et al. (2014), [4] TIMASS survey Caux et al. (2011), and [5] this work.
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