TASS Mark IV Photometric Survey of the Northern Sky

By T. Droege, M. Richmond, M. Sallman, Robert P. Creager. 2006

139 citations recorded by the source corpus.

The Amateur Sky Survey (TASS) is a loose confederation of amateur and professional astronomers. We describe the design and construction of our Mark IV systems, a set of wide‐field telescopes with CCD cameras that take simultaneous images in the V and IC passbands. We explain our observational procedures and the pipeline that processes and reduces the images into lists of stellar positions and magnitudes. We have compiled a large database of measurements for stars in the northern celestial hemisphere with V‐band magnitudes in the range 7<V<13. This paper describes data taken over the 4 year period beginning in 2001 November. One of our results is a catalog of repeated measurements on the Johnson‐Cousins system for over 4.3 million stars.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/742e11a89e4e734b2b73486d2c3e4512e6f91370

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Citations in the corpus

HAT-P-16b: A 4 MJ PLANET TRANSITING A BRIGHT STAR ON AN ECCENTRIC ORBIT, (2010, unknown): “56s, δ = +42◦27′47.1′′; J2000; V = 10.812; Droege et al. 2006), with a depth of ∼ 10.2mmag, and a period of P = 2.7760days.”
HAT-P-11b: A SUPER-NEPTUNE PLANET TRANSITING A BRIGHT K STAR IN THE KEPLER FIELD (2009, unknown): “As regards apparent magnitude, the TASS (Droege et al. 2006) photometry for this star is VTASS = 9.587 ± 0.071 and ITASS = 8.357± 0.050, yielding (V − I)TASS = 1.230 ± 0.087.”
HD 147506b: A Supermassive Planet in an Eccentric Orbit Transiting a Bright Star (2007, methodology): “Based on the Hipparcos parallax (π = 7.39±0.88mas), the apparent magnitude V = 8.71 ± 0.01 (Droege et al. 2006), the SME temperature, and a bolometric correction of BCV = −0.011± 0.011mag (Flower 1996), application of the Stefan-Boltzmann law yields a stellar radius of R⋆ = 1.84 ± 0.24 R⊙.”
DISCOVERY OF A TRANSITING PLANET AND EIGHT ECLIPSING BINARIES IN HATNet FIELD G205 (2009, methodology): “We have compared the (V − I )YY color to published observational data, and found that our model color agrees well with the observed TASS color of (V − I )TASS = 0.62 ± 0.09 (see Droege et al. 2006).”
ON THE METAL RICHNESS OF M DWARFS WITH PLANETS (2009, methodology): “We searched the VizieR online catalog (Ochsenbein et al. 2000) for alternative photometric measurements for these 7 stars, and located V -band photometry for 6 of them, mostly from the TYCHO/Hipparcos and TASS Mark IV Survey catalogs (Perryman & ESA 1997; Droege et al. 2006).”
HAT-P-7b: An Extremely Hot Massive Planet Transiting a Bright Star in the Kepler Field (2008, unknown): “◦8, the model color agrees well with the observed TASS color of (V − I)TASS = 0.60 ± 0.07 (see Droege et al. 2006).”