Photoelectric photometry - an approach to data reduction

Harris, W. E.; Fitzgerald, Mike; Reed, B. Cameron

doi:10.1086/130868

Cited by 89 publications

(76 citation statements)

References 6 publications

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“…We adopted 0.015 mag as the floor to the calculated errors, based on the observed dispersion in the transformation between instrumental and standard magnitudes of bright stars (see below). To derive the transformation of the instrumental magnitudes into the standard system, we used the following (Harris et al 1981):…”

Section: Optical Imagingmentioning

confidence: 99%

The Carnegie Supernova Project: The Low‐Redshift Survey

Hamuy

Folatelli

Morrell

et al. 2006

PUBL ASTRON SOC PAC

283

233

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ABSTRACT. Supernovae are essential to understanding the chemical evolution of the universe. Type Ia supernovae also provide the most powerful observational tool currently available for studying the expansion history of the universe and the nature of dark energy. Our basic knowledge of supernovae comes from the study of their photometric and spectroscopic properties. However, the presently available data sets of optical and nearinfrared light curves of supernovae are rather small and/or heterogeneous, and employ photometric systems that are poorly characterized. Similarly, there are relatively few supernovae whose spectral evolution has been well sampled, both in wavelength and phase, with precise spectrophotometric observations. The low-redshift portion of the Carnegie Supernova Project (CSP) seeks to remedy this situation by providing photometry and spectrophotometry of a large sample of supernovae taken on telescope/filter/detector systems that are well understood and well characterized. During a 5 year program that began in 2004 September, we expect to obtain high-precision uЈgЈrЈiЈBVYJHK s light curves and optical spectrophotometry for about 250 supernovae of all types. In this paper we provide a detailed description of the CSP survey observing and data reduction methodology. In addition, we present preliminary photometry and spectra obtained for a few representative supernovae during the first observing campaign.

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Section: Optical Imagingmentioning

confidence: 99%

The Carnegie Supernova Project: The Low‐Redshift Survey

Hamuy

Folatelli

Morrell

et al. 2006

PUBL ASTRON SOC PAC

283

233

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“…The standard star magnitudes were measured with PSF photometry and aperture corrections were applied to convert the PSF magnitudes to magnitudes in an aperture with a radius of five times the seeing. Following Harris et al (1981), all measured magnitudes were fitted simultaneously (with 3σ clipping) to derive linear transformation equations, with the additional requirement that the color-terms and the zero-points to be the same for the two nights. Second-order extinction terms were not included.…”

Section: Optical Photometrymentioning

confidence: 99%

SN 2003du: 480 days in the life of a normal type Ia supernova

Stanishev¹,

Goobar²,

Benetti

et al. 2007

A&A

163

156

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Aims. We present a study of the optical and near-infrared (NIR) properties of the Type Ia Supernova (SN Ia) 2003du.Methods. An extensive set of optical and NIR photometry and low-resolution long-slit spectra was obtained using a number of facilities. The observations started 13 days before B-band maximum light and continued for 480 days with exceptionally good time sampling. The optical photometry was calibrated through the S-correction technique. Results. The UBVRIJHK light curves and the color indices of SN 2003du closely resemble those of normal SNe Ia. SN 2003du reached a B-band maximum of 13.49 ± 0.02 mag on JD2 452 766.38 ± 0.5. We derive a B-band stretch parameter of 0.988 ± 0.003, which corresponds to ∆m 15 = 1.02 ±0.05, indicative of a SN Ia of standard luminosity. The reddening in the host galaxy was estimated by three methods, and was consistently found to be negligible. Using an updated calibration of the V and JHK absolute magnitudes of SNe Ia, we find a distance modulus µ = 32.79 ± 0.15 mag to the host galaxy, UGC 9391. We measure a peak uvoir bolometric luminosity of 1.35(±0.20) × 10 43 erg s −1 and Arnett's rule implies that M56 Ni 0.68 ± 0.14 M of 56 Ni was synthesized during the explosion. Modeling of the uvoir bolometric light curve also indicates M56 Ni in the range 0.6−0.8 M . The spectral evolution of SN 2003du at both optical and NIR wavelengths also closely resembles normal SNe Ia. In particular, the Si ii ratio at maximum R(Si ii) = 0.22 ± 0.02 and the time evolution of the blueshift velocities of the absorption line minima are typical. The pre-maximum spectra of SN 2003du showed conspicuous high-velocity features in the Ca ii H&K doublet and infrared triplet, and possibly in Si ii λ6355, lines. We compare the time evolution of the profiles of these lines with other well-observed SNe Ia and we suggest that the peculiar pre-maximum evolution of Si ii λ6355 line in many SNe Ia is due to the presence of two blended absorption components.

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“…Table 3 presents the best fit (computed using a linear single-value decomposition algorithm) to the photometric equation (e.g., Harris et al 1981):…”

Section: Calibrationmentioning

confidence: 99%

The Clustering of Galaxies around Threez∼ 3 Damped Lyα Absorbers

Bouché

Lowenthal

2004

ApJ

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We present our results on the cross-correlation of Lyman break galaxies ( LBGs) around three damped Ly absorbers ( DLAs) at z abs ' 3 from deep [ I; AB (sky) ' 27:6 mag arcsec À2 ] UBVI KPNO 4 m/ MOSAIC images. The large area of the MOSAIC images, 0.31 deg 2 or $65 ; 65 h À1 71 Mpc comoving at redshift z ¼ 3, allows us to probe the clustering of LBGs on scales up to 20 Mpc comoving. Our survey covers a total of 1 deg 2 and contains $3000 LBGs with photometric redshifts between 2.8 and 3.5. Using the redshift likelihood distributions with m I as a prior, we selected LBGs within a redshift slice of width W z ¼ 0:15 (corresponding to z , the uncertainty in photometric redshifts) centered on the redshift of the absorbers. Within that redshift slice, we find that the DLA-LBG cross-correlation w dg is w dg ¼ (1:62 AE 1:32) ; w gg , where w gg is the LBG autocorrelation. This corresponds to a correlation length of r 0 ¼ 5 AE 4:5 h À1 (comoving) (or r 0 ¼ 7 AE 6:8 h À171 Mpc). The cross-correlation is most significant on scales 5-10 Mpc. Through Monte Carlo simulations, we find that w dg is significantly greater than zero at the greater than 95% level. In three other redshift slices that do not contain a DLA, we do not find any evidence of clustering. A larger sample will enable us to discriminate between w dg =w gg < 1 and w dg =w gg > 1, i.e., to test whether DLA halos are more or less massive than LBG halos.

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Photoelectric photometry - an approach to data reduction

Cited by 89 publications

References 6 publications

The Carnegie Supernova Project: The Low‐Redshift Survey

The Carnegie Supernova Project: The Low‐Redshift Survey

SN 2003du: 480 days in the life of a normal type Ia supernova

The Clustering of Galaxies around Threez∼ 3 Damped Lyα Absorbers

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