2MASS All Sky Catalog of point sources.

By R. Cutri, M. Skrutskie, S. V. Dyk, C. Beichman, J. Carpenter, T. Chester, L. Cambrésy, T. Evans, J. Fowler, J. Gizis and 15 more. 2003

1,375 citations recorded by the source corpus.

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Citations in the corpus

• STELLAR AND PLANETARY PROPERTIES OF K2 CAMPAIGN 1 CANDIDATES AND VALIDATION OF 17 PLANETS, INCLUDING A PLANET RECEIVING EARTH-LIKE INSOLATION (2015, methodology): “We also record the J, H, and K magnitudes and their uncertainties as found in the 2MASS All-sky Catalog of Point Sources (Cutri et al. 2003) and the W W1 3- WISE magnitudes and uncertainties from the ALLWise Data Release (Cutri et al. 2013).”
• A Massive Cluster of Red Supergiants at the Base of the Scutum-Crux Arm (2007, methodology): “Therefore, in order to identify potential RSGs, we compiled a list of candidate stars within an 70 radius of the cluster center (as defined by Stephenson 1990) based on their Ks-band magnitudes in the TwoMicronAll Sky Survey (2MASS) point-source catalog (Cutri et al. 2003).”
• Characterization of the K2-18 multi-planetary system with HARPS: A habitable zone super-Earth and discovery of a second, warm super-Earth on a non-coplanar orbit (2017, background): “With J = 9.8, H = 9.1, and K = 8.9 (Cutri et al. 2003), we stress that K2-18 is currently the second brightest M dwarf with a transiting habitable zone planet behind the recently discovered LHS 1140b.”
• Herbig Ae/Be Stars in nearby OB Associations (2004, methodology): “We calculated fluxes for each H emission star using the B, V, Ic (ESA 1997) and J, H, KS (Cutri et al 2003) magnitudes corrected by reddening and the flux density for Vega (Cox 2000) at each band.”
• ε Indi Ba,Bb: The nearest binary brown dwarf (2003, methodology): “Adopted near-IR magnitudes for the combinedε Indi Ba,Bb system from the 2MASS Point Source Catalog (Cutri et al. 2003) and the derived individual magnitudes for the two components.”
• High-Resolution Submillimeter Constraints on Circumstellar Disk Structure (2006, methodology): “…that is a power law in frequency and independent of radius, ¼ 0 0 ; ð3Þ the flux density (F ) at any frequency can be determined by summing the thermal emission from annuli weighted by the optical depth ( ;r ¼ r), F ¼ cos i d 2 Z Rd r0 B Trð Þ 1 e ; r sec i 2 r dr; ð4Þ where i is the disk…”
• Small vs. large dust grains in transitional disks: do different cavity sizes indicate a planet? - SAO 206462 (HD 135344B) in polarized light with VLT/NACO (2013, unknown): “Parameter Value Right ascension (J2000) 15h 15m 48s.44 a Declination (J2000) -37◦ 09′ 16′′.03 a J [mag] 7.279± 0.026 b H [mag] 6.587± 0.031 b Ks [mag] 5.843± 0.020 b Visual extinctionAV [mag] 0.3 c Spectral type F4Ved Luminosity 7.8 L⊙ c Mass 1.7 M⊙ e Radius 1.4 R⊙ e Temperature 6810 Ke Mass accreti”
• Spitzer IRS Spectroscopy of IRAS-discovered Debris Disks (2006, unknown): “TD1 fluxes (Thompson et al. 1978) are plotted as pentagons; General Catalogue of Photometric Data mean UBV or Johnson et al. (1966) fluxes are plotted as triangles; and 2MASS JHK fluxes (Cutri et al. 2003) are plotted as squares.”
• Chandra Orion Ultradeep Project: Observations and Source Lists (2004, methodology): “2003), the approach adopted here is to discard events at the core of the PSF, which are both spatially and spectrally distorted, and to use only ordinary, pile-up–free events in the outskirts of the PSF (Broos et al. 1998).”