1 / 17

PMOD 13.7m CO Observations toward SNRs G54.1+0.3 & G22.7-0.2

PMOD 13.7m CO Observations toward SNRs G54.1+0.3 & G22.7-0.2. 2009.9.26-2009.11.04 Yang Su. Observations. Date: 9.26-11.04, 5-7 hours/day (260 hours) Weather condition: 200-270 K Ta r.m.s.~0.2-0.3 K/minute 12CO/13CO/C18O: 0.37/0.11/0.11 km/s Pointing: <3’’ for southern sky

sen
Download Presentation

PMOD 13.7m CO Observations toward SNRs G54.1+0.3 & G22.7-0.2

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  1. PMOD 13.7m CO Observations toward SNRs G54.1+0.3 & G22.7-0.2 2009.9.26-2009.11.04 Yang Su

  2. Observations • Date: 9.26-11.04, 5-7 hours/day (260 hours) • Weather condition: 200-270 K • Ta r.m.s.~0.2-0.3 K/minute • 12CO/13CO/C18O: 0.37/0.11/0.11 km/s • Pointing: <3’’ for southern sky • Tracking: ~1-3’’ • Main beam efficiency: 62%@90GHz

  3. AOS: • FFTS:

  4. Aims: a, To investigate the MC environment around SNRs; b, To study the association between SNRs and the ambient star forming regions (e.g., HII regions; H2CO,H2O & CH3OH masers; Young stellar clusters); • Method: • Using 12CO/13CO/C18O (J=1-0) spectral and spatial information to obtain the stable/unstable gas distribution and the kinematic velocity or distance of MCs; • Using HCO+(J=1-0)@89.18853GHz to identify the shock-MC regions; • Using HI 21cm & HISA to confine the source’s distance; • Using Spitzer MIPS/IRAC IR data to study the emissions of dust, PAH, molecular and atomic lines.

  5. Background: SNR G54.1+0.3 Observations: We mapped the 3.5’*3.5’ area (r.m.s~0.2K) centered at the PSR position (the cross in the figures) with grid spacing 0.5’ (half beam). For the remnant area (2R~2’), the noise is less than 0.1K for the three CO lines. Aims: Is there any 12CO broadening or intensity distribution to show the shock interaction in the region of the IR loop? Koo et al. 2008: The AKARI 15um and Spitzer 5.8um emission enhancement (or the IR loop in the southwest of the remnant) indicate that the star formation triggered by some mechanism. Is it because of the Massive Progenitor’s Wind of the remnant?

  6. Results: SNR G54.1+0.3 Thick:12CO Thin:13CO*2 Dashed: C18O*3 Focus on: A:[-10,0] km/s B:[0,6] km/s C:[7,12] km/s D:[17,28] km/s E:[49,57] km/s 3’*3’ centered at PSR D No correlation with SNR E A B C

  7. B D • The 12CO distribution centered at the PSR position • Upper-left:[1,4] km/s • Upper-right:[22,25] km/s • Lower-left:[52,55] km/s E

  8. Results: SNR G54.1+0.3 Blue shift • The 12-28 km/s MC wing (12CO) D Red shift

  9. Conclusions: SNR G54.1+0.3 • For 1-4 km/s MC, it seems surrounding the southwestern region of the remnant but no 12CO broadening; • For [52,55] km/s MC, it located at the eastern and southern part of the remnant; • For [22,24] km/s MC, the MC core covers the remnant but the 12CO broadening emission is ~1’ far from the radio boundary of the remnant. • HISA analysis of MCs are needed because of d(SNR)>d(tangent point); • HCO+ observations are needed in the regions of IR loop;

  10. Background: SNR G22.7-0.2 HII B Masers HII D Strong 5.8um emission surrounding the remnant Black Contours: C18O (71-82km/s) White Contours: 1.4G Radio HII A: RRL not to be detected HII B: 71.2km/s; d~10.3kpc HII C: 105-111km/s; d~7.4kpc HII D: 70.9km/s; 4.4kpc HII E: 74.1km/s; 4.6kpc HII F: 74.8km/s; 4.6kpc Masers (H2O,H2CO,CH3OH): 74.8km/s; 4.6 (4.26-4.97)kpc HII A HII E HII C HII F HI A or MC A HI B or MC B Aims 1: Are these star forming regions associated with the remnant?

  11. HI A: SNR bright Shell 1 Observations: We mapped the 43’*35’ area (r.m.s~0.2K) centered at the geometric center of the remnant with grid spacing 2’. For the shell structure (or the IR bright regions), the noise is about 0.15K and grid spacing 1’. Aims 2: Are there any MCs to associate with the remnant? Note:the velocity we are interested in should be less than 85km/s. HI B: SNR bright Shell 2

  12. Concave structure 12CO 68-70km/s+radio MC B HII region F MC A 5.8um+13CO (74-80km/s) contours 1.4 GHz radio emission 13CO*5 The MC shell structure along the radio periphery & probably the 12CO broadening

  13. Given the good spatial correlation between the MC complex, the HII regions and the radio boundary of the remnant, we believe that all of them are probably physically contacted with SNR.

  14. Conclusions: SNR G22.7-0.2 • The 77 km/s MC is likely associated with the remnant: 1,The MC A (east) is coincident well with the SNR’s radio shell; 2,The MC B (center and south, N(H)>2E22cm-2) is likely corresponding to the darkness of the IR emission; 3,The 12CO shell (v=68-70km/s; 13CO is weak) is surrounding the southeastern quarter of the remnant (in there IR 5.8um emission is strong); • HI absorption for the remnant and HISA analysis for MCs suggest that the remnant is less than 5.1 kpc (85km/s) and probably at 4.7kpc (77km/s; the near side of the Scutum arm); • The surrounding HII regions (D, E, & F) are likely associated with the remnant because of their similar distances. They were likely triggered by the massive progenitor’s wind of SNR; • Very interesting is that, the eastern shell of the remnant displays prominent “concave structure”. And HII region F is just located ~2’ east of the SNR radio “concave structure”. • HCO+ observations are needed in the regions of radio/IR peak;

  15. Thanks

More Related