Properties of M31. Ii. A Cepheid Disk Sample Derived From the First Year of Ps1 Pandromeda Data

Kodric, M.; Riffeser, A.; Hopp, U.; Seitz, S.; Koppenhoefer, J.; Bender, Ralf; Goessl, Claus; Snigula, J.; Lee, Chien‐Hsiu; Ngeow, Chow-Choong; Chambers, K.; Magnier, E. A.; Price, P. A.; Burgett, W. S.; Hodapp, Klaus W.; Kaiser, Nick; Kudritzki, Rolf‐Peter

doi:10.1088/0004-6256/145/4/106

Cited by 27 publications

(73 citation statements)

References 55 publications

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“…The prewhitening of the light curve is illustrated in Figure 1 An et al (2004) found the period of this star to be 9.42 days. The photometry presented by Kodric et al (2013) results in a primary period of 9.3918(85) days and a secondary period of 6.5551(49) days. The prewhitening of the light curve is presented in Figure 2.…”

Section: J00450019+4129313 -1o/2o Type Pulsatormentioning

confidence: 87%

“…The second set of light curves was presented by Kodric et al (2013). They analyzed data collected by the 1.8 m Panoramic Survey Telescope and Rapid Response System (Pan-STARRS) with the 1.4 × 10 9 pixel camera.…”

Section: Data and Methods Descriptionmentioning

confidence: 99%

“…The 183 epochs in the r P1 and i P1 bands (Tonry Cepheids were found including type II objects and variables that could not be definitely assigned to type I or type II. A more detailed description of the observation and their analysis was presented by Lee et al (2012) and Kodric et al (2013). Both Vilardell et al (2007) and Kodric et al (2013) used difference image analysis to perform photometric measurements.…”

Section: Data and Methods Descriptionmentioning

confidence: 99%

“…Using Kodric et al (2013) photometry we found periods of 9.1633(80) days and 6.3618(61) days (Figure 3). This object turns out to have periods similar to PSO_J010.6063+40.8608 discussed above, with a slightly smaller period ratio of 0.694.…”

Section: Pso_j0109364+412504 -F/1o Type Pulsatormentioning

confidence: 97%

“…Except for these stars, double mode Cepheids are known only in the Milky Way and M33 (Beaulieu et al 2006). There are also more than 2000 known Cepheids in the Andromeda galaxy (M31; Fliri & Valls-Gabaud 2012; Kodric et al 2013) and until now none of them has been claimed as a double mode pulsator.…”

Section: Introductionmentioning

confidence: 99%

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Double Mode Cepheids in M31

Poleski¹

2013

ApJ

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Until now, double mode Cepheids (or beat Cepheids) were known only in the Galaxy, the Magellanic Clouds, and M33. Curiously, none of the more than 2000 Cepheids in M31 was claimed to show two pulsation modes. We conducted a systematic search for double mode Cepheids in the archival data of M31 and discovered four such objects. We identify one of the stars as a first and second overtone pulsator even though its secondary period is subject to strong aliasing. Two stars pulsate in the fundamental mode and the first overtone. Their fundamental periods are 9.392 days and 9.163 days. This makes them the first candidates for fundamental mode and first overtone Cepheids, of which double mode pulsations are caused by the 2:1 resonance of the fundamental mode and the second overtone.

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Section: J00450019+4129313 -1o/2o Type Pulsatormentioning

confidence: 87%

Section: Data and Methods Descriptionmentioning

confidence: 99%

Section: Data and Methods Descriptionmentioning

confidence: 99%

Section: Pso_j0109364+412504 -F/1o Type Pulsatormentioning

confidence: 97%

Section: Introductionmentioning

confidence: 99%

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Double Mode Cepheids in M31

Poleski¹

2013

ApJ

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The 64 Mpixel wide field imager for the Wendelstein 2m telescope: design and calibration

et al. 2014

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The Wendelstein Observatory of Ludwig Maximilians University of Munich has recently been upgraded with a modern 2m robotic telescope. One Nasmyth port of the telescope has been equipped with a wide-field corrector which preserves the excellent image quality (< 0.8" median seeing) of the site (Hopp et al. 2008) over a field of view of 0.7 degrees diameter. The available field is imaged by an optical imager (WWFI, the Wendelstein Wide Field Imager) built around a customized 2 × 2 mosaic of 4k × 4k 15 µm e2v CCDs from Spectral Instruments. This paper provides an overview of the design and the WWFI's performance. We summarize the system mechanics (including a structural analysis), the electronics (and its electromagnetic interference (EMI) protection) and the control software. We discuss in detail detector system parameters, i.e. gain and readout noise, quantum efficiency as well as charge transfer efficiency (CTE) and persistent charges. First on sky tests yield overall good predictability of system throughput based on lab measurements.

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Period–luminosity–metallicity relation of classical Cepheids

Ripepi

Catanzaro

Molinaro

et al. 2020

A&A

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Context. Classical Cepheids (DCEPs) are the most important primary indicators for the extragalactic distance scale. Establishing the dependence on metallicity of their period–luminosity and period–Wesenheit (PL and PW) relations has deep consequences for the estimate of the Hubble constant (H0). Aims. We investigate the dependence on metal abundance ([Fe/H]) of the PL and PW relations for Galactic DCEPs. Methods. We combined proprietary and literature photometric and spectroscopic data, gathering a total sample of 413 Galactic DCEPs (372 fundamental mode, DCEP_F, and 41 first-overtone, DCEP_1O) and constructed new metallicity-dependent PL and PW relations in the near-infrared adopting the astrometry-based luminosity. Results. We find indications that the slopes of the PL(KS) and PW(J, KS) relations for Galactic DCEPs might depend on metallicity on the basis of the comparison with the Large Magellanic Cloud relationships. Therefore we used a generalized form of the PL and PW relations to simultaneously take the metallicity dependence of the slope and intercept of these relations into account. Conclusions. We calculated PL and PW relations that for the first time explicitly include a metallicity dependence of the slope and intercept terms. The quality of the available data is insufficient, however, and we cannot yet present conclusive results, but they are relevant from a methodological point of view. The new relations are linked to the geometric measurement of the distance to the Large Magellanic Cloud and allowed us to estimate a Gaia DR2 parallax zero-point offset Δϖ = 0.0615 ± 0.004 mas from the dataset of DCEPs used in this work.

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Properties of M31. Ii. A Cepheid Disk Sample Derived From the First Year of Ps1 Pandromeda Data

Cited by 27 publications

References 55 publications

Double Mode Cepheids in M31

Double Mode Cepheids in M31

The 64 Mpixel wide field imager for the Wendelstein 2m telescope: design and calibration

Period–luminosity–metallicity relation of classical Cepheids

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