Abstract
The Palomar Transient Factory (PTF) and its successor, the intermediate PTF (iPTF), are wide-field synoptic sky surveys aimed to detect transients. Even though the main science goal for PTF/iPTF is to detect various types of transients, the synoptic nature of the surveys can also be used for the study of variable stars. In this proceedings contribution, I will first give a brief introduction to PTF/iPTF, followed by the two pulsating stars studies using the PTF/iPTF data: the Ultra-Long Period Cepheids (ULPC) in M31 and the RR Lyrae in the Kepler field. For the formal study, we searched the M31’s ULPC using PTF imaging data, and follow up the candidates with other telescopes. Our finding revealed that there are only two ULPC in M31. I will give a brief implication of our finding in distance scale studies. For the latter study, I will present our work on the derivation of metallicity-light curve relation in native PTF/iPTF R-band using the RRab stars in the Kepler field.
Highlights
The 48-inch Samuel Oschin Telescope, known as P48, located at the Palomar Observatory, possesses a distinct history in modern observational astronomy
The P48 Telescope has been used in various surveys in the past, including the Palomar Observatory Sky Survey (POSS), the Near-Earth Asteroid Tracking (NEAT) program, and the Quasar Equatorial Survey Team (QUEST)
The Palomar Transient Factory (PTF)/intermediate PTF (iPTF) surveys employed a mixed cadence for their time series observations, ranging from few minutes to few days, that depends on various experiments
Summary
The 48-inch Samuel Oschin Telescope, known as P48, located at the Palomar Observatory, possesses a distinct history in modern observational astronomy. The fully robotic P48 is used for dedicated wide-field transients surveys, known as the Palomar Transient Factory (PTF, 2009-2012, [1, 2]) and intermediate-PTF (iPTF, 2013-2017). Both PTF and iPTF use the same wide-field mosaic camera, which consists of eleven 2K × 4K CCDs, equipped on the P48 to produce a field-of-view (FOV) of ∼ 7.3 degree-squared with a pixel scale of 1.01 /pixel. Besides the studies of transients – the main science goals of PTF/iPTF –, the time series PTF/iPTF data has been used in the variable stars research with noticeable examples presented in [3,4,5,6,7,8,9,10,11,12]. I present another two examples of using the PTF/iPTF data in pulsating variable stars works: the study of ultra-long period Cepheids (ULPC) and RR Lyrae
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