ApJ, in press

1999

Citations in the corpus

• A SYSTEMATIC SEARCH FOR TRANSITING PLANETS IN THE K2 DATA (2015, methodology): “They will also deliver input data for next-generation population inferences (Foreman-Mackey et al. 2014), especially for the population of planets around cool stars (for example, Dressing & Charbonneau 2015).”
• DISCOVERY OF AN ACTIVE GALACTIC NUCLEUS DRIVEN MOLECULAR OUTFLOW IN THE LOCAL EARLY-TYPE GALAXY NGC 1266 (2011, methodology): “2008), as well as the range of SFRs observed in the SAURON and ATLAS sample galaxies (Shapiro et al. 2010; Falcón-Barroso et al. in prep). The star formation-driven wind model of Murray et al. (2005) requires that the star formation rate be equal to or greater than the mass outflow rate for radiatio”
• EPISODIC ACCRETION AT EARLY STAGES OF EVOLUTION OF LOW-MASS STARS AND BROWN DWARFS: A SOLUTION FOR THE OBSERVED LUMINOSITY SPREAD IN H–R DIAGRAMS? (2009, background): “Several theoretical scenarios have been suggested to explain phases of non-steady accretion (Kenyon & Hartmann 1995; Vorobyov & Basu 2005; Zhu et al. 2008; Tassis & Muschovias 2005).”
• X-Ray Emission from Extragalactic Jets (2006, background): “Small angles to the line of sight and physical length of jets From recent quasar surveys with the CXO (Marshall et al. 2005, Sambruna et al. 2004, Schwartz et al. 2006), fitting IC/CMB models yield δ values which range from 3 to 11.”
• A Comprehensive Analysis of Swift XRT Data. II. Diverse Physical Origins of the Shallow Decay Segment (2007, methodology): “The plateau and the sharp drop in the XRT light curve of GRB 070110 is similar to that of GRB 060607A, but an additional “normal”decay component post the steep fall-off was also observed (Troja et al. 2007). The decay slope of this late X-ray emission component is similar to that of the optical ligh”
• Measurement of Galaxy Cluster Sizes, Radial Profiles, and Luminosity Functions from SDSS Photometric Data (2004, result): “For maxBCG clusters that have been found in the simulations of Wechsler et al. (2005), we find something similar: Ngals ∼ N 0.”
• A Test of the Collisional Dark Matter Hypothesis from Cluster Lensing (2000, background): “A second problem is that the number of dwarf galaxies observed in the Local Group is much smaller than the total number predicted from numerical simulations (Klypin et al. 1999 ; Moore et al. 1999b).”
• HOW DO DISKS SURVIVE MERGERS? (2008, methodology): “INTRODUCTION In the now established “concordance”ΛCDM cosmology, structure grows hierarchically (e.g. White & Rees 1978), making mergers and interactions between galaxies an essential and inescapable process in galaxy formation.”
• Mid-Infrared Galaxy Classification Based on Silicate Obscuration and PAH Equivalent Width (2006, methodology): “Archival ISO-SWSspectra of starburst nuclei were taken from Sturm et al. (2000). The Spitzerobservations were made with the Short-Low (SL) and Long-Low (LL) modules of theIRS.”
• X-ray spectral survey with XMM-Newton of a complete sample of nearby Seyfert galaxies (2005, methodology): “The XMM–Newton observation of this source was published by Kinkhabwala et al. (2002), who focused their analysis on the RGS study, and by Matt et al. (2004), who focused their analysis on the E > 4 keV data.”
• The Insignificance of P-R drag in detectable extrasolar planetesimal belts (2005, background): “It is worth noting that of the disks which have been resolved, those with ages ∼ 10 Myr all have η0 > 1000 (β Pic, HR4796, HD141569) while those older than 100 Myr all have η0 < 100 (Vega, ǫ Eridani, Fomalhaut, η Corvi). The fact that the debris disks which have been detected to date have η0 ≫ 1 imp”