New Cepheid Period-Luminosity Relations for the Large Magellanic Cloud: 92 Near-Infrared Light Curves

By S. E. Persson, B. Madore, W. Krzemiński, W. Freedman, M. Roth, D. Murphy. 2004

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In Astronomy and Astrophysics

Citations in the corpus

CARNEGIE HUBBLE PROGRAM: A MID-INFRARED CALIBRATION OF THE HUBBLE CONSTANT (2012, methodology): “Riess et al. adopt a distance modulus to the LMC of 18.486 ± 0.076 based on the Cepheid H-band sample of Persson et al. (2004), and measurements of eclipsing binaries.”
A REDETERMINATION OF THE HUBBLE CONSTANT WITH THE HUBBLE SPACE TELESCOPE FROM A DIFFERENTIAL DISTANCE LADDER (2009, methodology): “For the sample we find bH = −3.09 ± 0.11, in good agreement with the value of −3.23 ± 0.04 from the LMC (Persson et al. 2004).”
THE CARNEGIE SUPERNOVA PROJECT: FIRST PHOTOMETRY DATA RELEASE OF LOW-REDSHIFT TYPE Ia SUPERNOVAE (2009, methodology): “For this task, we have chosen a variation of the “gloess” algorithm (Madore 2001), which is a Gaussian-windowed and error-weighted extension of data-smoothing methods outlined by Cleveland (1979), and first implemented by Persson et al. (2004) for fitting Cepheid light curves.”
A New Calibration Of Galactic Cepheid Period-Luminosity Relations From B To K Bands, And A Comparison To LMC Relations (2007, methodology): “In the infrared, we will use both the Persson et al. (2004) relations based on 92 Cepheids with well-sampled light curves (22 phase points per star on average), and an OGLE sample 4 ftp://sirius.astrouw.edu.pl/ogle/ogle2/var stars/lmc/cep/catalog/ README.”
New Parallaxes of Galactic Cepheids from Spatially Scanning the Hubble Space Telescope: Implications for the Hubble Constant (2018, background): “…to be seen with the Hubble Space Telescope (HST) in the hosts of nearby SNeIa (D≈ 20–40 Mpc), and they yield an individual distance precision of 0.07 mag (Persson et al. 2004; Macri et al. 2015) when observed in the NIR, where they are also insensitive to metallicity (Wielgorski et al. 2017).”
Cepheid parallaxes and the Hubble constant (2007, background): “The LMC relations of Persson et al. (2004) converted to the SAAO system using the relations of Carter (1990) are: K0 = −3.258 log P + 16.048 (9) and K0 = −3.457 log P + 1.894(J − K)0 + 15.402.”
Hubble Space Telescope Fine Guidance Sensor Parallaxes of Galactic Cepheid Variable Stars: Period-Luminosity Relations (2006, methodology): “The LMC distance moduli in Table 15 from the Persson et al. (2004)K data in x 6.3 suggest that the metallicity correction may be smaller for K than for WVI.”
A 3% SOLUTION: DETERMINATION OF THE HUBBLE CONSTANT WITH THE HUBBLE SPACE TELESCOPE AND WIDE FIELD CAMERA 3 (2011, methodology): “…of a reliable and precise distance to the LMC. Guinan et al. (1998), Fitzpatrick et al. (2002), and Ribas et al. (2002) studied three B-type systems (HV2274, HV982, and EROS1044) which lie close to the bar of the LMC and therefore provide a good match to the Cepheid sample of Persson et al. (2004).”
THE CARNEGIE SUPERNOVA PROJECT: LIGHT-CURVE FITTING WITH SNooPy (2010, methodology): “The GLOESS algorithm (Persson et al. 2004), a variant of the more well-known LOESS (Cleveland et al. 1991) interpolator, is therefore appropriate in this case and we use a 2- dimensional extension which we call GLOESS2D.”
H 0 revisited (2013, methodology): “(4b) The upper period limit is imposed because there is evidence that the P-L relation departs from a power law for periods >∼ 60 days (Persson et al., 2004; Freedman et al. 2011; Scowcroft et al.2011).”
A 2.4% DETERMINATION OF THE LOCAL VALUE OF THE HUBBLE CONSTANT (2016, background): “…et al. (2015) presented NIR photometry for LMC Cepheids discovered by the OGLE-III project (Soszynski et al. 2008), greatly expanding the sample size relative to that of Persson et al. (2004) from 92 to 785, although the number of Cepheids with P>10 days increased more modestly from 39 to 110.”
THE CARNEGIE SUPERNOVA PROJECT: ANALYSIS OF THE FIRST SAMPLE OF LOW-REDSHIFT TYPE-Ia SUPERNOVAE (2009, methodology): “…point in the three-dimensional space, we use a two-dimensional variation of the “gloess” algorithm, which is a Gaussian-windowed and error-weighted extension of data-smoothing methods outlined by Cleveland (1979) that was first implemented by Persson et al. (2004) for fitting Cepheid light curves.”