V440 Per: the longest-period overtone Cepheid

Baranowski, R.; Smolec, R.; Dimitrov, W.; Kwiatkowski, T.; Schwarzenberg‐Czerny, A.; Bartczak, P.; Fagas, M.; Borczyk, W.; Kamiński, K.; Moskalik, P.; Ratajczak, R.; Rożek, A.

doi:10.1111/j.1365-2966.2009.14865.x

Cited by 25 publications

(25 citation statements)

References 13 publications

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“…V340 Nor (P ∼ 11 d ) is a fundamental mode pulsator, since overtone pulsators terminate near 7 d in the Magellanic Clouds Soszyñski et al 2008, see the latter's Figs. 5 & 6), and the longest-period overtone pulsator known in the Galaxy may be V440 Per (7.57 d , Baranowski et al 2009). For QZ Nor (P ∼ 4 d ) the matter is more complicated.…”

Section: Radial Velocitiesmentioning

confidence: 99%

Anchors for the cosmic distance scale: the Cepheid QZ Normae in the open cluster NGC 6067

Majaess¹,

Sturch

Bidin

et al. 2013

Astrophys Space Sci

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Cepheids are key to establishing the cosmic distance scale. Therefore it's important to assess the viability of QZ Nor, V340 Nor, and GU Nor as calibrators for Leavitt's law via their purported membership in the open cluster NGC 6067. The following suite of evidence confirms that QZ Nor and V340 Nor are members of NGC 6067, whereas GU Nor likely lies in the foreground: (i) existing radial velocities for QZ Nor and V340 Nor agree with that established for the cluster (−39.4 ± 0.2(σx) ± 1.2(σ) km/s) to within 1 km/s, whereas GU Nor exhibits a markedly smaller value; (ii) a steep velocity-distance gradient characterizes the sight-line toward NGC 6067, thus implying that objects sharing common velocities are nearly equidistant; (iii) a radial profile constructed for NGC 6067 indicates that QZ Nor is within the cluster bounds, despite being 20 ′ from the cluster center; (iv) new BV JH photometry for NGC 6067 confirms the cluster lies d = 1.75 ± 0.10 kpc distant, a result that matches Wesenheit distances computed for QZ Nor/V340 Nor using the Benedict et al. (2007, HST parallaxes) calibration. QZ Nor is a cluster Cepheid that should be employed as a calibrator for the cosmic distance scale.

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Section: Radial Velocitiesmentioning

confidence: 99%

Anchors for the cosmic distance scale: the Cepheid QZ Normae in the open cluster NGC 6067

Majaess¹,

Sturch

Bidin

et al. 2013

Astrophys Space Sci

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“…However, the Fourier parameters of RV curves are indistinguishable for fundamental and first‐overtone pulsators with periods around 5 d (see fig. 3 of Baranowski et al 2009). Light curve Fourier parameters suffer from similar problems.…”

Section: V1154 Cyg the Only Kepler Cepheidmentioning

confidence: 97%

Cepheid investigations using the Kepler space telescope

Szabo¹,

Szabados²,

Ngeow³

et al. 2011

Monthly Notices of the Royal Astronomical Society

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We report results of initial work done on selected candidate Cepheids to be observed with the Kepler space telescope. Prior to the launch 40 candidates were selected from previous surveys and databases. The analysis of the first 322 days of Kepler photometry, and recent ground-based follow-up multicolour photometry and spectroscopy allowed us to confirm that one of these stars, V1154 Cyg (KIC 7548061), is indeed a 4.9-d Cepheid. Using the phase lag method we show that this star pulsates in the fundamental mode. New radial velocity data are consistent with previous measurements, suggesting that a long-period binary component is unlikely. No evidence is seen in the ultra-precise, nearly uninterrupted Kepler photometry for nonradial or stochastically excited modes at the micromagnitude level. The other candidates are not Cepheids but an interesting mix of possible spotted stars, eclipsing systems and flare stars.Comment: 13 pages, 15 figures, accepted for publication in MNRAS, electronic-only tables are available upon request from the first autho

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“…To confirm the detection of the four components we started observations on the new 0.4 m Poznan Spectroscopic Telescope 1 (PST 1) equipped with fiber fed echelle spectrograph (detailed description in Baranowski et al 2009). Its high photon efficiency allows RV measurements for objects as faint as 11 mag.…”

Section: Spectroscopymentioning

confidence: 99%

Spectroscopy of HD 86222 – a quintuple system with an eclipsing component

Dimitrov

Fagas

Kamiński

et al. 2014

A&A

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We present spectroscopic and photometric analysis of the quintuple star HD 86222 with an eclipsing component. Until now three visual components A, B, and C of this multiple star were known. Four components in the A/B pair were detected during the examination of the cross correlation functions obtained from the spectra. We noticed that the visual components A and B, separated by 0. 5, are in fact two binary stars -one eclipsing pair and one spectroscopic system. The pair with higher radial velocity amplitude corresponds to the eclipsing period. Photometric and spectroscopic observations of the eclipsing binary enable us to obtain the Wilson-Devinney model. The masses of this pair are M 1 = 1.29 ± 0.09 M and M 2 = 1.33 ± 0.09 M , respectively. The radii, slightly higher than for the main sequence stars, are R 1 = 1.35 ± 0.01 R and R 2 = 1.36 ± 0.01 R , respectively. The main parameters of the spectroscopic binary are also estimated, but they must be confirmed by future observations because of the uncertainty of the period. The farthest star named C, is 15 arc seconds from the main A and B components. Assuming that this object is gravitationally connected with the A and B binary pairs, HD 86222 has at least five components.

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V440 Per: the longest-period overtone Cepheid

Cited by 25 publications

References 13 publications

Anchors for the cosmic distance scale: the Cepheid QZ Normae in the open cluster NGC 6067

Anchors for the cosmic distance scale: the Cepheid QZ Normae in the open cluster NGC 6067

Cepheid investigations using the Kepler space telescope

Spectroscopy of HD 86222 – a quintuple system with an eclipsing component

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