Kenneth W. Cavagnolo, Ph.D. - Publications

Affiliations: 
2008 Michigan State University, East Lansing, MI 
Area:
Astronomy and Astrophysics

8 high-probability publications. We are testing a new system for linking publications to authors. You can help! If you notice any inaccuracies, please sign in and mark papers as correct or incorrect matches. If you identify any major omissions or other inaccuracies in the publication list, please let us know.

Year Citation  Score
2009 Cavagnolo KW, Donahue M, Voit GM, Sun M. Intracluster medium entropy profiles for a chandra archival sample of galaxy clusters Astrophysical Journal, Supplement Series. 182: 12-32. DOI: 10.1088/0067-0049/182/1/12  0.6
2008 Cavagnolo KW, Donahue M, Voit GM, Sun M. An entropy threshold for strong ha and radio emission in the cores of galaxy clusters Astrophysical Journal. 683. DOI: 10.1086/591665  0.681
2008 Voit GM, Cavagnolo KW, Donahue M, Rafferty DA, McNamara BR, Nulsen PEJ. Conduction and the star formation threshold in brightest cluster galaxies Astrophysical Journal. 681. DOI: 10.1086/590344  0.633
2008 Cavagnolo KW, Donahue M, Voit GM, Sun M. Bandpass Dependence of X-Ray Temperatures in Galaxy Clusters The Astrophysical Journal. 682: 821-834. DOI: 10.1086/588630  0.607
2007 Donahue M, Ming S, O'Dea CP, Mark Voit G, Cavagnolo KW. Star formation, radio sources, cooling x-ray gas, and galaxy interactions in the brightest cluster galaxy in 2A0335+096 Astronomical Journal. 134: 14-25. DOI: 10.1086/518230  0.65
2007 Sharpee B, Zhang Y, Williams R, Pellegrini E, Cavagnolo K, Baldwin JA, Phillips M, Liu X. s-PROCESS ABUNDANCES IN PLANETARY NEBULAE The Astrophysical Journal. 659: 1265-1290. DOI: 10.1086/511665  0.425
2006 Donahue M, Horner DJ, Cavagnolo KW, Voit GM. Entropy profiles in the cores of cooling flow clusters of galaxies Astrophysical Journal. 643: 730-750. DOI: 10.1086/503270  0.645
2006 Zhang Y, Williams R, Pellegrini E, Cavagnolo K, Baldwin JA, Sharpee B, Phillips M, Liu X-. Abundances of s-process elements in planetary nebulae: Br, Kr & Xe Arxiv: Astrophysics. 2: 549-550. DOI: 10.1017/S1743921306004182  0.342
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