J/AJ/130/2453 9 high-redshift ESSENCE supernovae (Krisciunas+, 2005)
Hubble space telescope observations of nine high-redshift ESSENCE supernovae.
Krisciunas K., Garnavich P.M., Challis P., Prieto J.L., Riess A.G.,
Barris B., Aguilera C., Becker A.C., Blondin S., Chornock R.,
Clocchiatti A., Covarrubias R., Filippenko A.V., Foley R.J., Hicken M.,
Jha S., Kirshner R.P., Leibundgut B., Li W., Matheson T., Miceli A.,
Miknaitis G., Rest A., Salvo M.E., Schmidt B.P., Smith R.C., Sollerman J.,
Spyromilio J., Stubbs C.W., Suntzeff N.B., Tonry J.L., Wood-Vasey W.M.
<Astron. J., 130, 2453-2472 (2005)>
=2005AJ....130.2453K 2005AJ....130.2453K
ADC_Keywords: Supernovae ; Redshifts ; Photometry, HST ; Photometry, VRI
Keywords: distance scale - galaxies: distances and redshifts -
supernovae: general
Abstract:
We present broadband light curves of nine supernovae ranging in
redshift from 0.5 to 0.8. The supernovae were discovered as part of
the ESSENCE project, and the light curves are a combination of Cerro
Tololo 4m and Hubble Space Telescope (HST) photometry. On the basis
of spectra and/or light-curve fitting, eight of these objects are
definitely Type Ia supernovae, while the classification of one is
problematic. The ESSENCE project is a 5yr endeavor to discover about
200 high-redshift Type Ia supernovae, with the goal of tightly
constraining the time average of the equation-of-state parameter
[w=p/(ρc2)] of the "dark energy." To help minimize our
systematic errors, all of our ground-based photometry is obtained with
the same telescope and instrument. In 2003 the highest redshift subset
of ESSENCE supernovae was selected for detailed study with HST. Here
we present the first photometric results of the survey.
Description:
In this paper we report photometry of nine objects discovered in 2003
October, November, and December, which were also observed with HST ACS
(using the Wide Field Camera). The goal of the HST observations was to
observe the highest redshift end of the ESSENCE sample, since
photometry becomes difficult with the CTIO 4m as they fade. In Table
1 we list the nine objects. Their redshifts were obtained from
observations with the Keck I Low Resolution Imaging Spectrometer
(LRIS), Gemini Multiobject Spectrograph (GMOS), VLT FORS1, or Magellan
(Baade + Inamori Magellan Areal Camera and Spectrograph [IMACS]).
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 50 9 High-redshift SNe: basic data
table2.dat 82 49 HST photometry
table3.dat 54 101 Ground-based R and I photometry
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See also:
B/sn : Asiago Supernova Catalogue (Barbon et al., 1999-)
J/ApJ/594/1 : High-z supernovae VRI mag and distances (Tonry+, 2003)
J/ApJ/602/571 : High-redshift supernovae IRZ fluxes (Barris+, 2004)
J/ApJ/613/200 : Hubble Higher z Supernova Search, HHZSS (Strolger+, 2004)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 9 A9 --- Name SN name
11- 14 A4 --- ESSENCE ESSENCE name
16- 17 I2 h RAh Hour of Right Ascension (J2000.0)
19- 20 I2 min RAm Minute of Right Ascension (J2000.0)
22- 26 F5.2 s RAs Second of Right Ascension (J2000.0)
28 A1 --- DE- Sign of the Declination (J2000.0)
29- 30 I2 deg DEd Degree of Declination (J2000.0)
32- 33 I2 arcmin DEm Arcminute of Declination (J2000.0)
35- 38 F4.1 arcsec DEs Arcsecond of Declination (J2000.0)
40- 43 F4.2 --- z Redshift (1)
44 A1 --- f_z Flag on z (2)
46- 50 F5.3 mag E(B-V) From the reddening maps of Schlegel et al.
(1998ApJ...500..525S 1998ApJ...500..525S)
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Note (1): Obtained from the spectra of the SNe themselves, rather than the
host galaxies. We used our program SNID (J. L. Tonry et al. 2006, in
preparation).
Note (2): Flag on z, defined as follows:
c = See text and Matheson et al. (2005AJ....129.2352M 2005AJ....129.2352M) for a
discussion of the redshift of this object
d = The minimum reduced χ2 value of the light-curve fits
is obtained for z=0.68; no spectroscopic redshift was obtained
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Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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1- 9 A9 --- Name SN name
11- 20 F10.2 --- JD Julian Date
22- 27 F6.3 mag F625W ? HST/ACS F625W band magnitude (1)
29- 32 F4.2 mag E_F625W ? Upper 1σ error in F625W (2)
34- 38 F5.3 mag e_F625W ? The 1σ error in F625W
40- 45 F6.3 mag F775W ? HST/ACS F775W band magnitude (1)
47- 50 F4.2 mag E_F775W ? Upper 1σ error in F775W (2)
52- 56 F5.3 mag e_F775W ? The 1σ error in F775W
58- 63 F6.3 mag F850LP ? HST/ACS F850W band magnitude (1)
65- 69 F5.3 mag e_F850LP ? The 1σ error in F850LP
71- 76 F6.3 mag F110W ? HST/NICMOS F110W band magnitude
78- 82 F5.3 mag e_F110W ? The 1σ error in F110W
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Note (1): The ACS magnitudes given are "Vega" magnitudes derived using
50-pixel-radius zeropoints (Sirianni et al. 2005PASP..117.1049S 2005PASP..117.1049S),
which are based on the Vega spectrophotometric calibration of
Bohlin & Gilliland (2004AJ....127.3508B 2004AJ....127.3508B).
Note (2): When this value is given the data in the following column
represents the lower 1σ error.
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Byte-by-byte Description of file: table3.dat
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Bytes Format Units Label Explanations
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1- 9 A9 --- Name SN name
11- 20 F10.2 --- JD Julian Date
22 A1 --- l_Rmag Indicates Rmag is a 1σ upper limit
23- 27 F5.2 mag Rmag ? The R band magnitude (1)
29- 32 F4.2 mag E_Rmag ? Upper 1σ error in Rmag (2)
34- 37 F4.2 mag e_Rmag ? The 1σ error in Rmag
39 A1 --- l_Imag Indicates Imag is a 1σ upper limit
40- 44 F5.2 mag Imag ? The I band magnitude (1)
46- 49 F4.2 mag E_Imag ? Upper 1σ error in Imag (2)
51- 54 F4.2 mag e_Imag ? The 1σ error in Imag
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Note (1): The magnitudes are natural system "Vega" magnitudes.
See text for more details.
Note (2): When this value is given the data in the following column
represents the lower 1σ error.
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History:
From electronic version of the journal
(End) Greg Schwarz [AAS], Marianne Brouty [CDS] 20-Apr-2006