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Kevin Krisciunas,
Deepak Bastola,
Juan Espinoza,
David Gonzalez,
Luis Gonzalez, Sergio Gonzalez,
Mario Hamuy,
Eric Y. Hsiao,
Nidia Morrell,
Mark M. Phillips,
Nicholas B. Suntzeff
[show abstract]
[hide abstract]
ABSTRACT: We present previously unpublished photometry of supernovae 2003gs and 2003hv.
Using spectroscopically-derived corrections to the U-band photometry, we
reconcile U-band light curves made from imagery with the Cerro Tololo 0.9-m,
1.3-m and Las Campanas 1-m telescopes. Previously, such light curves showed a
0.4 mag spread at one month after maximum light. This gives us hope that a set
of corrected ultraviolet light curves of nearby objects can contribute to the
full utilization of rest frame U-band data of supernovae at redshift ~0.3 to
0.8. As pointed out recently by Kessler et al. in the context of the Sloan
Digital Sky Survey supernova search, if we take the published U-band photometry
of nearby Type Ia supernovae at face value, there is a 0.12 mag U-band anomaly
in the distance moduli of higher redshift objects. This anomaly led the Sloan
survey to eliminate from their analyses all photometry obtained in the rest
frame U-band. The Supernova Legacy Survey eliminated observer frame U-band
photometry, which is to say nearby objects observed in the U-band, but they
used photometry of high redshift objects no matter in which band the photons
were emitted.
11/2012;
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Maximilian D. Stritzinger,
M. M. Phillips,
Luis N. Boldt,
Chris Burns,
Abdo Campillay,
Carlos Contreras, Sergio Gonzalez,
Gastón Folatelli,
Nidia Morrell,
Wojtek Krzeminski, [......],
Mario Hamuy,
Wendy L. Freedman,
Barry F. Madore,
J. L. Marshall,
Sven E. Persson,
Jean-Philippe Rheault,
Nicholas B. Suntzeff,
Steven Villanueva,
Weidong Li,
and Alexei V. Filippenko
[show abstract]
[hide abstract]
ABSTRACT: The Carnegie Supernova Project (CSP) was a five-year observational survey conducted at Las Campanas Observatory that obtained, among other things, high-quality light curves of ~100 low-redshift Type Ia supernovae (SNe Ia). Presented here is the second data release of nearby SN Ia photometry consisting of 50 objects, with a subset of 45 having near-infrared follow-up observations. Thirty-three objects have optical pre-maximum coverage with a subset of 15 beginning at least five days before maximum light. In the near-infrared, 27 objects have coverage beginning before the epoch of B-band maximum, with a subset of 13 beginning at least five days before maximum. In addition, we present results of a photometric calibration program to measure the CSP optical (uBgVri) bandpasses with an accuracy of ~1%. Finally, we report the discovery of a second SN Ia, SN 2006ot, similar in its characteristics to the peculiar SN 2006bt.
The Astronomical Journal 10/2011; 142(5):156. · 4.03 Impact Factor
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Maximilian Stritzinger,
M. M. Phillips,
Luis Boldt S,
Chris Burns,
Abdo Campillay,
Carlos Contreras, Sergio Gonzalez,
Gaston Folatelli,
Nidia Morrell,
Wojtek Krzeminski, [......],
Mario Hamuy,
Wendy L. Freedman,
Barry Madore,
Jennifer L. Marshall,
Sven E. Persson,
Jean-Philippe Rheault,
Nicholas Suntzeff,
Steven Villanueva,
Weidong Li,
Alexei V. Filippenko
[show abstract]
[hide abstract]
ABSTRACT: The Carnegie Supernova Project (CSP) was a five-year observational survey
conducted at Las Campanas Observatory that obtained, among other things,
high-quality light curves of ~100 low-redshift Type Ia supernovae (SNe Ia).
Presented here is the second data release of nearby SN Ia photometry consisting
of 50 objects, with a subset of 45 having near-infrared follow-up observations.
Thirty-three objects have optical pre-maximum coverage with a subset of 15
beginning at least 5 days before maximum light. In the near-infrared, 27
objects have coverage beginning before the epoch of B-band maximum, with a
subset of 13 beginning at least 5 days before maximum. In addition, we present
results of a photometric calibration program to measure the CSP optical
(uBgVri)bandpasses with an accuracy of ~1%. Finally, we report the discovery of
a second SN Ia, SN 2006ot, similar in its characteristics to the peculiar SN
2006bt.
08/2011;
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Kevin Krisciunas,
Weidong Li,
Thomas Matheson,
D. Andrew Howell,
Maximilian Stritzinger,
Greg Aldering,
Perry L. Berlind,
M. Calkins,
Peter Challis,
Ryan Chornock, [......],
Peter E. Nugent,
M. Phelps,
Mark M. Phillips,
Yulei Qiu,
Robert Quimby,
K. Rines,
Jeffrey M. Silverman,
Nicholas B. Suntzeff,
Rollin C. Thomas,
Lifan Wang
[show abstract]
[hide abstract]
ABSTRACT: We present optical and near-infrared photometry, as well as ground-based
optical spectra and Hubble Space Telescope ultraviolet spectra, of the Type Ia
supernova (SN) 2001ay. At maximum light the Si II and Mg II lines indicated
expansion velocities of 14,000 km/sec, while Si III and S II showed velocities
of 9,000 km/sec There is also evidence for some unburned carbon at 12,000
km/sec. SN 2001ay exhibited a decline-rate parameter Delta m_15(B) = 0.68 \pm
0.05 mag; this and the B-band photometry at t > +25 d past maximum make it the
most slowly declining Type Ia SN yet discovered. Three of four
super-Chandrasekhar-mass candidates have decline rates almost as slow as this.
After correction for Galactic and host-galaxy extinction, SN 2001ay had M_B =
-19.19 and M_V = -19.17 mag at maximum light; thus, it was not overluminous in
optical bands. In near-infrared bands it was overluminous only at the 2-sigma
level at most. For a rise time of 18 d (explosion to bolometric maximum) the
implied Ni-56 yield was (0.58 \pm 0.15)/alpha M_Sun, with alpha = L_max/E_Ni
probably in the range 1.0 to 1.2. The Ni-56 yield is comparable to that of many
Type Ia supernovae. The "normal" Ni-56 yield and the typical peak optical
brightness suggest that the very broad optical light curve is explained by the
trapping of the gamma rays in the inner regions.
06/2011;
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Christopher R. Burns,
Maximilian Stritzinger,
M. M. Phillips,
ShiAnne Kattner,
S. E. Persson,
Barry F. Madore,
Wendy L. Freedman,
Luis Boldt,
Abdo Campillay,
Carlos Contreras,
Gaston Folatelli, Sergio Gonzalez,
Wojtek Krzeminski,
Nidia Morrell,
Francisco Salgado,
and Nicholas B. Suntzeff
[show abstract]
[hide abstract]
ABSTRACT: In providing an independent measure of the expansion history of the universe, the Carnegie Supernova Project (CSP) has observed 71 high-z Type Ia supernovae (SNe Ia) in the near-infrared bands Y and J. These can be used to construct rest-frame i-band light curves which, when compared to a low-z sample, yield distance moduli that are less sensitive to extinction and/or decline-rate corrections than in the optical. However, working with NIR observed and i-band rest-frame photometry presents unique challenges and has necessitated the development of a new set of observational tools in order to reduce and analyze both the low-z and high-z CSP sample. We present in this paper the methods used to generate uBVgriYJH light-curve templates based on a sample of 24 high-quality low-z CSP SNe. We also present two methods for determining the distances to the hosts of SN Ia events. A larger sample of 30 low-z SNe Ia in the Hubble flow is used to calibrate these methods. We then apply the method and derive distances to seven galaxies that are so nearby that their motions are not dominated by the Hubble flow.
The Astronomical Journal 12/2010; 141(1):19. · 4.03 Impact Factor
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[show abstract]
[hide abstract]
ABSTRACT: A trend is emerging regarding the progenitor stars that give rise to the most common core-collapse supernovae (SNe), those of Type II-Plateau (II-P): they generally appear to be red supergiants with a limited range of initial masses, ~8-16 M ☉. Here, we consider another example, SN 2008cn, in the nearly face-on spiral galaxy NGC 4603. Even with limited photometric data, it appears that SN 2008cn is not a normal SN II-P, but is of the high-luminosity subclass. Through comparison of pre- and post-explosion images obtained with the Wide Field and Planetary Camera 2 on board the Hubble Space Telescope, we have isolated a supergiant star prior to explosion at nearly the same position as the SN. We provide evidence that this supergiant may well be the progenitor of the SN, although this identification is not entirely unambiguous. This is exacerbated by the distance to the host galaxy, 33.3 Mpc, making SN 2008cn the most distant SN II-P yet for which an attempt has been made to identify a progenitor star in pre-SN images. The progenitor candidate has a more yellow color ([V – I]0 = 0.98 mag and T eff = 5200 ± 300 K) than generally would be expected and, if a single star, would require that it exploded during a "blue loop" evolutionary phase, which is theoretically not expected to occur. Nonetheless, we estimate an initial mass of M ini = 15 ± 2 M ☉ for this star, which is within the expected mass range for SN II-P progenitors. The yellower color could also arise from the blend of two or more stars, such as a red supergiant and a brighter, blue supergiant. Such a red supergiant hidden in this blend could instead be the progenitor and would also have an initial mass within the expected progenitor mass range. Furthermore, the yellow supergiant could be in a massive, interacting binary system, analogous to the possible yellow supergiant progenitor of the high-luminosity SN II-P 2004et. Finally, if the yellow supergiant is not the progenitor, or is not a stellar blend or binary containing the progenitor, then we constrain any undetected progenitor star to be a red supergiant with M ini 11 M ☉, considering a physically more realistic scenario of explosion at the model endpoint luminosity for a rotating star.
The Astrophysical Journal 11/2009; 706(2):1174. · 6.02 Impact Factor
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Kevin Krisciunas,
G. H. Marion,
Nicholas B. Suntzeff,
Guillaume Blanc,
Filomena Bufano,
Pablo Candia,
Regis Cartier,
Nancy Elias-Rosa,
Juan Espinoza,
David Gonzalez,
Luis Gonzalez, Sergio Gonzalez,
Samuel D. Gooding,
Mario Hamuy,
Ethan A. Knox,
Peter A. Milne,
Nidia Morrell,
Mark M. Phillips,
Maximilian Stritzinger,
and Joanna Thomas-Osip
[show abstract]
[hide abstract]
ABSTRACT: We obtained optical photometry of SN 2003gs on 49 nights, from 2 to 494 days after T(B max). We also obtained near-IR photometry on 21 nights. SN 2003gs was the first fast declining Type Ia SN that has been well observed since SN 1999by. While it was subluminous in optical bands compared to more slowly declining Type Ia SNe, it was not subluminous at maximum light in the near-IR bands. There appears to be a bimodal distribution in the near-IR absolute magnitudes of Type Ia SNe at maximum light. Those that peak in the near-IR after T(B max) are subluminous in the all bands. Those that peak in the near-IR prior to T(B max), such as SN 2003gs, have effectively the same near-IR absolute magnitudes at maximum light regardless of the decline rate Δm 15(B). Near-IR spectral evidence suggests that opacities in the outer layers of SN 2003gs are reduced much earlier than for normal Type Ia SNe. That may allow γ rays that power the luminosity to escape more rapidly and accelerate the decline rate. This conclusion is consistent with the photometric behavior of SN 2003gs in the IR, which indicates a faster than normal decline from approximately normal peak brightness.
The Astronomical Journal 10/2009; 138(6):1584. · 4.03 Impact Factor
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Mario Hamuy,
Jinsong Deng,
Paolo A. Mazzali,
Nidia I. Morrell,
Mark M. Phillips,
Miguel Roth, Sergio Gonzalez,
Joanna Thomas-Osip,
Wojtek Krzeminski,
Carlos Contreras, [......],
Luis González,
Leonor Huerta,
Gastón Folatelli,
Ryan Chornock,
Alexei V. Filippenko,
S. E. Persson,
W. L. Freedman,
Kathleen Koviak,
Nicholas B. Suntzeff,
and Kevin Krisciunas
[show abstract]
[hide abstract]
ABSTRACT: Optical and near-infrared photometry and optical spectroscopy are reported for SN 2003bg, starting a few days after explosion and extending for a period of more than 300 days. Our early-time spectra reveal the presence of broad, high-velocity Balmer lines. The nebular-phase spectra, on the other hand, show a remarkable resemblance to those of Type Ib/c supernovae, without clear evidence for hydrogen. Near maximum brightness SN 2003bg displayed a bolometric luminosity comparable to that of other Type I hypernovae unrelated to gamma-ray bursts, implying a rather normal amount of 56Ni production (0.1-0.2 M ☉) compared with other such objects. The bolometric light curve of SN 2003bg, on the other hand, is remarkably broad, thus suggesting a relatively large progenitor mass at the moment of explosion. These observations, together with the large value of the kinetic energy of expansion established in the accompanying paper, suggest that SN 2003bg can be regarded as a Type IIb hypernova.
The Astrophysical Journal 09/2009; 703(2):1612. · 6.02 Impact Factor
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Mario Hamuy,
Jinsong Deng,
Paolo A. Mazzali,
Nidia I. Morrell,
Mark M. Phillips,
Miguel Roth, Sergio Gonzalez,
Joanna Thomas-Osip,
Wojtek Krzeminski,
Carlos Contreras, [......],
Luis Gonzalez,
Leonor Huerta,
Gaston Folatelli,
Ryan Chornock,
Alexei V. Filippenko,
S. E. Persson,
W. L. Freedman,
Kathleen Koviak,
Nicholas B. Suntzeff,
Kevin Krisciunas
[show abstract]
[hide abstract]
ABSTRACT: Optical and near-infrared photometry and optical spectroscopy are reported for SN 2003bg, starting a few days after explosion and extending for a period of more than 300 days. Our early-time spectra reveal the presence of broad, high-velocity Balmer lines. The nebular-phase spectra, on the other hand, show a remarkable resemblance to those of Type Ib/c supernovae, without clear evidence for hydrogen. Near maximum brightness SN 2003bg displayed a bolometric luminosity comparable to that of other Type I hypernovae unrelated to gamma-ray bursts, implying a rather normal amount of 56Ni production (0.1-0.2 Msun) compared with other such objects. The bolometric light curve of SN 2003bg, on the other hand, is remarkably broad, thus suggesting a relatively large progenitor mass at the moment of explosion. These observations, together with the large value of the kinetic energy of expansion established in the accompanying paper (Mazzali et al. 2009), suggest that SN 2003bg can be regarded as a Type IIb hypernova. Comment: 41 pages, 12 figures, accepted by The Astrophysical Journal
08/2009;
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Maximilian Stritzinger,
Paolo Mazzali,
Mark M. Phillips,
Stefan Immler,
Alicia Soderberg,
Jesper Sollerman,
Luis Boldt,
Jonathan Braithwaite,
Peter Brown,
Christopher R. Burns, [......], Sergio Gonzalez,
Mario Hamuy,
Wojtek Krzeminski,
Barry F. Madore,
Peter Milne,
Nidia Morrell,
S. E. Persson,
Miguel Roth,
Mathew Smith,
Nicholas B. Suntzeff
[show abstract]
[hide abstract]
ABSTRACT: A detailed study spanning approximately a year has been conducted on the Type
Ib supernova 2007Y. Imaging was obtained from X-ray to radio wavelengths, and a
comprehensive set of multi-band (w2m2w1u'g'r'i'UBVYJHKs) light curves and
optical spectroscopy is presented. A virtually complete bolometric light curve
is derived, from which we infer a (56)Ni-mass of 0.06 M_sun. The early spectrum
strongly resembles SN 2005bf and exhibits high-velocity features of CaII and
H_alpha; during late epochs the spectrum shows evidence of a ejecta-wind
interaction. Nebular emission lines have similar widths and exhibit profiles
that indicate a lack of major asymmetry in the ejecta. Late phase spectra are
modeled with a non-LTE code, from which we find (56)Ni, O and total-ejecta
masses (excluding He) to be 0.06, 0.2 and 0.42 M_sun, respectively, below 4,500
km/s. The (56)Ni mass confirms results obtained from the bolometric light
curve. The oxygen abundance suggests the progenitor was most likely a ~3.3
M_sun He core star that evolved from a zero-age-main-sequence mass of 10-13
M_sun. The explosion energy is determined to be ~10^50 erg, and the mass-loss
rate of the progenitor is constrained from X-ray and radio observations to be
<~10^-6 M_sun/yr. SN 2007Y is among the least energetic normal Type Ib
supernovae ever studied.
02/2009;
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Kevin Krisciunas,
Mario Hamuy,
Nicholas B. Suntzeff,
Juan Espinoza,
David Gonzalez,
Luis Gonzalez, Sergio Gonzalez,
Kathleen Koviak,
Wojtek Krzeminski,
Nidia Morrell,
Mark M. Phillips,
Miguel Roth,
and Joanna Thomas-Osip
[show abstract]
[hide abstract]
ABSTRACT: We present infrared photometry of supernova (SN) 1999em, plus optical photometry, infrared photometry, and optical spectroscopy of SN 2003hn. Both objects were Type II-P SNe. The V – [RIJHK] color curves of these SNe evolved in a very similar fashion until the end of the plateau phase. This allows us to determine how much more extinction the light of SN 2003hn suffered compared to SN 1999em. Since we have an estimate of the total extinction suffered by SN 1999em from model fits of ground-based and space-based spectra as well as photometry of SN 1999em, we can estimate the total extinction and absolute magnitudes of SN 2003hn with reasonable accuracy. Since the host galaxy of SN 2003hn also produced the Type Ia SN 2001el, we can directly compare the absolute magnitudes of these two SNe of different types.
The Astronomical Journal 12/2008; 137(1):34. · 4.03 Impact Factor
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Kevin Krisciunas,
Mark M. Phillips,
Nicholas B. Suntzeff,
S. E. Persson,
Mario Hamuy,
Roberto Antezana,
Pablo Candia,
Alejandro Clocchiatti,
Darren L. DePoy,
Lisa M. Germany, [......],
José Maza,
Peter E. Nugent,
Yulei Qiu,
Armin Rest,
Miguel Roth,
Maximilian Stritzinger,
L.-G. Strolger,
Ian Thompson,
T. B. Williams,
and Marina Wischnjewsky
[show abstract]
[hide abstract]
ABSTRACT: We present near-infrared photometry of the Type Ia supernova (SN) 1999ee; also, optical and infrared photometry of the Type Ia SNe 2000bh, 2000ca, and 2001ba. For SNe 1999ee and 2000bh, we present the first-ever SN photometry at 1.035 μm (the Y band). We present K-corrections that transform the infrared photometry in the observer's frame to the supernova rest frame. Using our infrared K-corrections and stretch factors derived from optical photometry, we construct JHK templates that can be used to determine the apparent magnitudes at maximum if one has some data in the window -12 to +10 days with respect to T(Bmax). Following up previous work on the uniformity of V minus IR loci of Type Ia supernovae of midrange decline rates, we present unreddened loci for slow decliners. We also discuss evidence for a continuous change of color at a given epoch as a function of decline rate.
The Astronomical Journal 12/2007; 127(3):1664. · 4.03 Impact Factor
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Kevin Krisciunas,
Nicholas B. Suntzeff,
Pablo Candia,
José Arenas,
Juan Espinoza,
David Gonzalez, Sergio Gonzalez,
Peter A. Höflich,
Arlo U. Landolt,
Mark M. Phillips,
and Sergio Pizarro
[show abstract]
[hide abstract]
ABSTRACT: We present well-sampled optical (UBVRI) and infrared (JHK) light curves of the nearby (≈18.0 Mpc) Type Ia supernova SN 2001el, from 11 days before to 142 days after the time of B-band maximum. The data represent one of the best sets of optical and infrared photometry ever obtained for a Type Ia supernova (SN). Based on synthetic photometry using optical spectra of SN 2001el and optical and infrared spectra of SN 1999ee, we were able to devise filter corrections for the BVJHK photometry of SN 2001el, which to some extent resolve systematic differences between SN 2001el data sets obtained with different telescope/filter/instrument combinations. We also calculated V-minus-infrared color curves on the basis of a delayed detonation model and show that the theoretical color curves match the unreddened loci for Type Ia SNe with midrange decline rates to within 0.2 mag. Given the completeness of the light curves and the elimination of filter-oriented systematic errors to some degree, the data presented here will be useful for the construction of photometric templates, especially in the infrared. On the whole the photometric behavior of SN 2001el was quite normal. The second H-band maximum being brighter than the first H-band maximum is in accord with the prediction of Krisciunas et al. for Type Ia SNe with midrange decline rates. The photometry exhibits nonzero host extinction, with total AV = 0.57 ± 0.05 mag along the line of sight. NGC 1448, the host of SN 2001el, would be an excellent target for a distance determination using Cepheids.
The Astronomical Journal 12/2007; 125(1):166. · 4.03 Impact Factor
