Display data from paper

Data:

LIT11 - Search for class I methanol maser emission toward several supernova remnants

Short title: Litovchenko et al. (2011)
Authors: Litovchenko, I. D. Alakoz, A. V. Val'Tts, I. E. Larionov, G. M.
Journal: Astronomy Reports, Volume 55, Issue 11, pp.978-988
Bibcode:

PDF:

Target type: SNR
Transitions: SiO_1-0v0,CH3OH_36(I),CH3OH_44(I),CH3OH_95(I),CH3OH_132(I),CH3OH_6(II)

Abstract
Observations at 44 GHz in the 7₀-6₁ A ⁺ methanol line have been carried out on the 20-m telescope of the Onsala Space Observatory (Sweden) in the directions of the poorly studied region G27.4-0.2 and of several supernova remnants, at the coordinates of the OH(1720) maser satellite emission, with the aim of searching for Class I methanol maser emission in these sources. The region G27.4-0.2 has beenmapped, and contains maser sources and two supernova remnants with similar coordinates and radial velocities, which may accelerate condensation of the ambient gas-dust medium. This may play a role in enhancing the probability of methanol formation and maser emission. This is the first detection of 44 GHz maser emission in this source, and this maser is among the 10% of the strongest Class I methanol masers, within the uncertainties in the integrated flux (of a total of 198 currently knownmasers). A 27' × 27' region around the maser has been mapped at 44 GHz in steps of 1'. The 44-GHz emission forms only within the previously known maser region. Further studies in water lines are needed to estimate the influence of shocks from supernovae. No 44-GHz Class I methanol maser emission was detected at the 3 sigma level at the coordinates of the OH(1720) satellite emission in six supernova remnants i.e., the presence of OH(1720) emission is not a sufficient condition for the detection of Class I methanol masers.	Target sources: RA(J2000) = 18 41 50.90, Dec(J2000) = -05 01 28.3 Comments: Several supernova remnants

Abstract

Observations at 44 GHz in the 7₀-6₁ A ⁺ methanol line have been carried out on the 20-m telescope of the Onsala Space Observatory (Sweden) in the directions of the poorly studied region G27.4-0.2 and of several supernova remnants, at the coordinates of the OH(1720) maser satellite emission, with the aim of searching for Class I methanol maser emission in these sources. The region G27.4-0.2 has beenmapped, and contains maser sources and two supernova remnants with similar coordinates and radial velocities, which may accelerate condensation of the ambient gas-dust medium. This may play a role in enhancing the probability of methanol formation and maser emission. This is the first detection of 44 GHz maser emission in this source, and this maser is among the 10% of the strongest Class I methanol masers, within the uncertainties in the integrated flux (of a total of 198 currently knownmasers). A 27' × 27' region around the maser has been mapped at 44 GHz in steps of 1'. The 44-GHz emission forms only within the previously known maser region. Further studies in water lines are needed to estimate the influence of shocks from supernovae. No 44-GHz Class I methanol maser emission was detected at the 3 sigma level at the coordinates of the OH(1720) satellite emission in six supernova remnants i.e., the presence of OH(1720) emission is not a sufficient condition for the detection of Class I methanol masers.

Target sources:
RA(J2000) = 18 41 50.90, Dec(J2000) = -05 01 28.3

Comments:
Several supernova remnants

Input tables: Table 1
Download as: Table (CSV)
View paper statistics

Detection table from Litovchenko et al. (2011)

Export table to csv

Hide / Show individual components

Display associated data

Group name
Different Line detections
IRAS source	IRAS coordinates (RA, Dec)	IRAS source distance (arcsec)	IRAS flux density (F12,F25,F60,F100)
2MASS source	2MASS coordinates (RA, Dec)	2MASS source distance (arcsec)	2MASS magnituted (J,H,K)
GCVS source	GCVS coordinates (RA, Dec)	GCVS source distance (arcsec)	GCVS parameters
WISE source	WISE coordinates (RA, Dec)	WISE source distance (arcsec)	WISE magnitudes (w1, w2, w3, w4)
Akari IRC source	Akari IRC coordinates (RA, Dec)	Akari IRC source distance (arcsec)	Akari IRC fluxes (S09, S18)
Akari FIS source	Akari FIS coordinates (RA, Dec)	Akari FIS source distance (arcsec)	Akari FIS fluxes (S65, S90, S140, S160)
Continuum source	Continuum coordinates (RA, Dec)	Continuum source distance (arcsec)	Continuum parameters
Bolocam GPS	BGPS coordinates (RA, Dec)	BGPS source distance (arcsec)	BGPS parameters
EGO source	EGO coordinates (RA, Dec)	EGO source distance (arcsec)	EGO parameters
Select all	Select all	Select all	Select all

View images

DSS (optical)	2MASS (JHK)	WISE (4-22 um)	IRAC (3-8 um)	GLIMPSE 360 (3.6-4.5 um)	PACS color (70-160 um)	SPIRE color (250-500 um)
AKARI color (60-160 um)	NVSS (1.4 GHz)	SDSS (optical+NIR)	Image size: arcsec (default is 120 arcsec)
			Image size: arcsec (default is 120 arcsec)

Position of H₂O maser detection

DSS colored	2MASS colored	WISE colored
SDSS color	IRAC color I1,I2,I4	GLIMPSE 360
PACS color (70-160 um)	SPIRE color (250-500 um)	NVSS (1.4GHz)
UKIDSS K	2MASS K

select MAX(h2o_data.ra_hms) as ra_hms,MAX(h2o_data.dec_dms) as dec_dms,MAX(h2o_data.source_name) as source_name,MAX(h2o_data.ra) as ra,MAX(h2o_data.dec) as dec,MAX(h2o_data.l) as l,MAX(h2o_data.b) as b FROM h2o_data  WHERE ref ilike 'LIT11' AND detected=true AND hide=false GROUP BY ref

select h2o_data.ra_hms,h2o_data.dec_dms,h2o_data.source_name,h2o_data.ra,h2o_data.dec,h2o_data.l,h2o_data.b FROM h2o_data   WHERE ref ilike 'LIT11' AND detected=true AND hide=false ORDER BY detected DESC,id

Display data from paper

LIT11 - Search for class I methanol maser emission toward several supernova remnants

View paper statistics

Detection table from Litovchenko et al. (2011)