CO $\mathsf{J}=\mathsf{1}{-}0$ observations of gas near the galactic supernova remnants G5.4-1.2, G5.55+0.32 and G5.71-0.08

Abstract

Results. Although broad CO lines characteristic of shocked gas were not seen in this kinematically complex region, a bright (14 K), new, marginally-resolved ±9 km s −1 outflow source G5.638+0.233 and a comparably bright rim of CO emission were found at/around the periphery of SNR G5.55+0.12. Most of the periphery of SNR G5.71-0.08 is surrounded by a bright rim of CO emission. CO emission at the 7 km s −1 velocity of a 1720 OH maser spot near SNR G5.70-0.12 is very bright, 19 K, but gas at −21 km s −1 is widespread over the region and CO emission is rather weak toward the OH maser spots at this velocity north of G5.4-1.2. Other very bright CO lines in the region are associated with H II regions, i.e. 27 K toward W28A2 = G5.89-0.39 and 15 K toward an MSX-IR source at l = 5.9 o , b = −0.13 o which is probably the exciting agent of a separate, classical HII region just north of W28A2.

12 mm line survey of the dense molecular gas towards the W28 field TeV gamma-ray sources

“…In this way we show the intrinsic velocity location and width of the gas without confusion. Based on the PV maps, it is clear that much of the NH 3 emission is found in the velocity range of ∼−5 to ∼20 km s −1 which is quite consistent with the molecular gas found in CO studies (Aharonian et al 2008b; Fukui et al 2008; Liszt 2009) towards the W28 region. The four satellite lines of NH 3 (1,1) are clearly visible towards most of the cores as colocated peaks with 7 and 19 km s −1 separation from the main line for the inner and outer satellite lines, respectively.…”

“…Core 5 appears to straddle the south‐east quadrant of the 8 μm IR shell or excitation ring of G5.89−0.39A and HESS J1800−240B, and is resolved into two components Core 5 NE and SW. Local peaks in CO emission overlapping Core 5 NE and SW are clearly visible [see Fig. 6 and also Liszt (2009) and Kim & Koo (2003)]. Core 5 NE is the coldest of the cores detected with T k ∼ 12 K. Here we detect only NH 3 (1,1) emission in mapping, and only very weak (2,2) and (3,3) emission in the deep spectra.…”

“…Core 5 appears to straddle the south-east quadrant of the 8 μm IR shell or excitation ring of G5.89−0.39A and HESS J1800−240B, and is resolved into two components Core 5 NE and SW. Local peaks in CO emission overlapping Core 5 NE and SW are clearly visible [see Fig. 6 and also Liszt (2009) and Kim & Koo (2003)].…”

A Systematic Survey for Broadened Co Emission Toward Galactic Supernova Remnants

“…These effects are usually more severe in lower energy transitions where line emission from quiescent clouds is intrinsically broad. Indeed, both of the BML non-detections in Table 3 were performed in 12 CO J = 1 − 0 and toward SNRs near the Galactic Center (G5.4-1.2, G5.7-0.0) (Liszt 2009). Observations in higher energy transitions might show less emission from quiescent clouds along the line-of-sight while revealing broad-line emission.…”

Discovery of Broad Molecular Lines and of Shocked Molecular Hydrogen From the Supernova Remnant G357.7+0.3: Hhsmt, Apex, Spitzer, and Sofia Observations

“…Millimeter observations provide direct, unambiguous evidence of interaction when a broad (>10 km s −1 ) line caused by dynamic motion of shocked gas is detected. There has been a long-term effort to search for interactions with clouds using millimeter observations (Huang & Thaddeus 1986;Liszt 2009;Jeong et al 2013;Zhou & Chen 2011). However, detection of broad CO lines is still limited to a half-dozen SNRs.…”