THE M31 NEAR-INFRARED PERIOD-LUMINOSITY RELATION AND ITS NON-LINEARITY FOR δ Cep VARIABLES WITH 0.5 ⩽ log (<i>P</i>) ⩽ 1.7

Kodric, M.; Riffeser, A.; Seitz, S.; Snigula, J.; Hopp, U.; Lee, Chien‐Hsiu; Goessl, Claus; Koppenhoefer, J.; Bender, Ralf; Gieren, W.

doi:10.1088/0004-637x/799/2/144

Cited by 32 publications

(59 citation statements)

References 33 publications

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“…In comparison with the Cepheid P-L relation, the TRGB was used to measure distance to a much larger number of galaxies, including galaxies that lack young standard candles like classical Cepheids. Cepheid distance measurements are also affected by numerous systematic errors including reddening, a possible metallicity dependence, or a nonlinearity of the P-L relation (Kodric et al 2015). Therefore the TRGB method is an important tool that can complement and perhaps improve the determination of the Hubble parameter.…”

Section: Introductionmentioning

confidence: 99%

The Araucaria Project: Multi-band Calibrations of the TRGB Absolute Magnitude

Górski

Pietrzyński

Gieren

et al. 2018

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We present new empirical calibrations of the absolute magnitude of the tip of the red giant branch (TRGB) in the optical I and near-infrared J, H, and K bands in terms of the (V-K) 0 , (V-H) 0 , and (J-K) 0 colors of the red giant branch. Our calibrations are based on the measurements in 19 fields in the Large and Small Magellanic Clouds, which span a wide (V-K) 0 color range of the brightest part of the red giant branch. We use a simple edge detection technique based on the comparison of the star count difference in two adjacent bins with the estimated Poisson noise. Further, we include the reddening and geometrical corrections, as well as the precise and accurate to 2% distance to the Large Magellanic Cloud. The calibration based on a (V-K) colors can be a robust tool to calculate with a great precision the absolute magnitude of the TRGB.

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Section: Introductionmentioning

confidence: 99%

The Araucaria Project: Multi-band Calibrations of the TRGB Absolute Magnitude

Górski

Pietrzyński

Gieren

et al. 2018

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“…We All samples show no evidence of a broken slope. Previously in Kodric et al (2015) we found a significant broken slope. We find that the broken slope is caused by a subsample of Cepheids that have a different color from the other Cepheids and have a high extinction but are otherwise the same.…”

Section: Resultsmentioning

confidence: 64%

“…Riess et al (2012). Also shown are the slopes from Kodric et al (2013), Kodric et al (2015) and Kodric et al (2018a). The fits to the FM Cepheids shown in table 2, table 5 and table 8 are also shown.…”

Section: Resultsmentioning

confidence: 98%

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M31 PAndromeda Cepheid Sample Observed in Four HST Bands

Kodric

Riffeser

Seitz

et al. 2018

ApJ

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Using the M31 PAndromeda Cepheid sample and the HST PHAT data we obtain the largest Cepheid sample in M31 with HST data in four bands. For our analysis we consider three samples: A very homogeneous sample of Cepheids based on the PAndromeda data, the mean magnitude corrected PAndromeda sample and a sample complementing the PAndromeda sample with Cepheids from literature. The latter results in the largest catalog with 522 fundamental mode (FM) Cepheids and 102 first overtone (FO) Cepheids with F160W and F110W data and 559 FM Cepheids and 111 FO Cepheids with F814W and F475W data. The obtained dispersion of the Period-Luminosity relations (PLRs) is very small (e.g. 0.138 mag in the F160W sample I PLR). We find no broken slope in the PLRs when analyzing our entire sample, but we do identify a subsample of Cepheids that causes the broken slope. However, this effect only shows when the number of this Cepheid type makes up a significant fraction of the total sample. We also analyze the sample selection effect on the Hubble constant.

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“…The two most notable uses are the massive surveys of M33 (Hartman et al 2006) and M31 (Kodric et al 2013(Kodric et al , 2015 using the MMT and the Pan-STARRS telescopes, respectively. Unfortunately, despite concerted efforts over the past decade (Ribas et al 2005;Bonanos et al 2006;Vilardell et al 2010) neither galaxy has a distance estimate as robust as that for the LMC by Pietrzyński et al (2013)…”

Section: Fiducial Cepheid P-l Relations In Sdss Filtersmentioning

confidence: 99%

Cepheid Variables in the Maser-Host Galaxy NGC 4258

Hoffmann

Macri

2015

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We present results of a ground-based survey for Cepheid variables in NGC 4258. This galaxy plays a key role in the Extragalactic Distance Scale due to its very precise and accurate distance determination via very long baseline interferometry observations of water masers. We imaged two fields within this galaxy using the Gemini North telescope and the Gemini Multi-Object Spectrograph, obtaining 16 epochs of data in the Sloan Digital Sky Survey gri bands over 4 yr. We carried out point-spread function photometry and detected 94 Cepheids with periods between 7 and 127 days, as well as an additional 215 variables which may be Cepheids or Population II pulsators. We used the Cepheid sample to test the absolute calibration of theoretical gri Period-Luminosity relations and found good agreement with the maser distance to this galaxy. The expected data products from the Large Synoptic Survey Telescope should enable Cepheid searches out to at least 10 Mpc.

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THE M31 NEAR-INFRARED PERIOD-LUMINOSITY RELATION AND ITS NON-LINEARITY FOR δ Cep VARIABLES WITH 0.5 ⩽ log (P) ⩽ 1.7

Cited by 32 publications

References 33 publications

The Araucaria Project: Multi-band Calibrations of the TRGB Absolute Magnitude

The Araucaria Project: Multi-band Calibrations of the TRGB Absolute Magnitude

M31 PAndromeda Cepheid Sample Observed in Four HST Bands

Cepheid Variables in the Maser-Host Galaxy NGC 4258

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