GCM +0.20 -0.03 , the SIMBAD biblio

GCM +0.20 -0.03 , the SIMBAD biblio (12 results) C.D.S. - SIMBAD4 rel 1.8 - 2024.04.25CEST18:52:40


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Bibcode/DOI Score in Title|Abstract|
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in a table in teXt, Caption, ... Nb occurence Nb objects in ref Citations
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Title First 3 Authors
1994ApJ...424L..91S 2 8 87 The source of the relativistic particles in the Galactic Center Arc. SERABYN E. and MORRIS M.
1997A&A...317..441P 1 7 34 The Galactic Center arc as source of high energy γ-rays. POHL M.
1998A&A...335..161M 3 20 203 High-energy gamma-ray emission from the Galactic Center. MAYER-HASSELWANDER H.A., BERTSCH D.L., DINGUS B.L., et al.
2001ApJ...548L..65M 25 32 Large-scale grain mantle disruption in the Galactic Center. MARTIN-PINTADO J., RIZZO J.R., DE VICENTE P., et al.
2001PASJ...53..779O 10 22 A molecular cloud and an expanding cavity adjacent to the nonthermal filaments of the Galactic Center radio arc. OKA T., HASEGAWA T., SATO F., et al.
2005ApJ...626..174P 9 12 A variability and localization study of the galactic center gamma-ray source 3EG J1746-2851. POHL M.
2006A&A...455..971R viz 1 61 187 Organic molecules in the Galactic center. Hot core chemistry without hot cores. REQUENA-TORRES M.A., MARTIN-PINTADO J., RODRIGUEZ-FRANCO A., et al.
2007ApJ...670.1115S viz 20 26 Spitzer IRS observations of the Galactic Center: shocked gas in the radio arc bubble. SIMPSON J.P., COLGAN S.W.J., COTERA A.S., et al.
2017A&A...599A.136L 41           X         1 13 9 Kinematics and properties of the central molecular zone as probed with [C II]. LANGER W.D., VELUSAMY T., MORRIS M.R., et al.
2018ApJ...852...11B 3894 T   A S   X C       92 15 6
M0.20-0.033: an expanding molecular shell in the Galactic Center Radio Arc.
BUTTERFIELD N., LANG C.C., MORRIS M., et al.
2022ApJ...936..186B 314           X C       6 8 ~ Evidence for an Interaction between the Galactic Center Clouds M0.10-0.08 and M0.11-0.11. BUTTERFIELD N.O., LANG C.C., GINSBURG A., et al.
2024ApJ...962...39L 100             C       1 19 ~ Magnetic Fields in the Central Molecular Zone Influenced by Feedback and Weakly Correlated with Star Formation. LU X., LIU J., PILLAI T., et al.

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