DSpace Angular :: Browsing by Author "Prieto, J. L."

Browsing by Author "Prieto, J. L."

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CRTS: An Open Optical Transient Survey
(2011) Drake, Andrew J.; Djorgovski, S. G.; Mahabal, A.; Williams, R.; Graham, M. J.; Donalek, C.; Prieto, J. L.; Catelan, Márcio; Beshore, E.; Larson, S.; Christensen, E.
The Catalina Real-time Transient Survey (CRTS) is an open optical transient survey that covers 3/4 of the entire sky in a search of transient astrophysical phenomena occurring on timescales of minutes to years. Observational data is derived from the three telescopes of the Catalina Sky Survey which cover up to 2,500 square degrees of sky each night. CRTS has so far discovered more that 2000 transient sources including 600 supernovae, 500 dwarf novae and more than 100 Blazars and UV Ceti variables. All data is processed within minutes of observation and discoveries are openly distributed using SkyAlert and VOEvent technologies as well as iPhone, html tables, RSS and Twitter feeds. Events are classified utilizing data from virtual observatory enabled archives, machine learning, and collaborative Citizen science....
HIGH-AMPLITUDE δ-SCUTIS IN THE LARGE MAGELLANIC CLOUD
(2010) Garg, A.; Cook, K. H.; Nikolaev, S.; Huber, M. E.; Rest, A.; Becker, A. C.; Challis, P.; Clocchiatti, A.; Miknaitis, G.; Minniti, D.; Morelli, L.; Olsen, K.; Prieto, J. L.; Suntzeff, N. B.; Welch, D. L.; Wood-Vasey, W. M.
We present 2323 high-amplitude delta-Scuti (HADS) candidates discovered in the Large Magellanic Cloud by the SuperMACHO survey (Rest et al.). Frequency analyses of these candidates reveal that several are multimode pulsators, including 119 whose largest amplitude of pulsation is in the fundamental (F) mode and 19 whose largest amplitude of pulsation is in the first overtone (FO) mode. Using Fourier decomposition of the HADS light curves, we find that the period-luminosity (PL) relation defined by the FO pulsators does not show a clear separation from the PL relation defined by the F pulsators. This differs from other instability strip pulsators such as type c RR Lyrae. We also present evidence for a larger amplitude, subluminous population of HADS similar to that observed in Fornax.
Light echoes reveal an unexpectedly cool η Carinae during its nineteenth-century Great Eruption
(2012) Rest, A.; Prieto, J. L.; Walborn, N. R.; Smith, N.; Bianco, F. B.; Chornock, R.; Welch, D. L.; Howell, D. A.; Huber, M. E.; Foley, R. J.; Fong, W.; Sinnott, B.; Bond, H. E.; Smith, R. C.; Toledo, I.; Minniti, D.; Mandel, K.
eta Carinae is one of the most massive binary stars in the Milky Way(1,2). It became the second-brightest star in our sky during its mid-nineteenth-century 'Great Eruption', but then faded from view (with only naked-eye estimates of brightness(3,4)). Its eruption is unique in that it exceeded the Eddington luminosity limit for ten years. Because it is only 2.3 kiloparsecs away, spatially resolved studies of the nebula have constrained the ejected mass and velocity, indicating that during its nineteenth-century eruption, eta Car ejected more than ten solar masses in an event that released ten per cent of the energy of a typical core-collapse supernova(5,6), without destroying the star. Here we report observations of light echoes of eta Carinae from the 1838-1858 Great Eruption. Spectra of these light echoes show only absorption lines, which are blueshifted by -210 km s(-1), in good agreement with predicted expansion speeds(6). The light-echo spectra correlate best with those of G2-to-G5 supergiants, which have effective temperatures of around 5,000 kelvin. In contrast to the class of extragalactic outbursts assumed to be analogues of the Great Eruption of eta Carinae(7-12), the effective temperature of its outburst is significantly lower than that allowed by standard opaque wind models(13). This indicates that other physical mechanisms such as an energetic blast wave may have triggered and influenced the eruption.
Luminous Type II supernovae for their low expansion velocities
(2020) Rodríguez, O.; Pignata, Giuliano; Anderson, J. P.; Moriya, T. J.; Clocchiatti, Alejandro; Förster, F.; Prieto, J. L.; Phillips, M. M.; Burns, C. R.; Contreras, C.; Folatelli, G.; Gutiérrez, C. P.; Hamuy, M.; Morrell, N. I.; Stritzinger, M. D.; Suntzeff, N. B.; Benetti, S.; Cappellaro, E.; Elias Rosa, N.; Pastorello, A.; Turatto, M.; Maza, J.; Antezana, R.; Cartier, R.; González, L.; Haislip, J. B.; Kouprianov, V.; López, P.; Marchi Lasch, S.; Reichart, D.
Massive stars exploding in a He-rich circumstellar medium - V. Observations of the slow-evolving SN Ibn OGLE-2012-SN-006
(2015) Pastorello, A.; Wyrzykowski, L.; Valenti, S.; Prieto, J. L.; Kozlowski, S.; Udalski, A.; Elias-Rosa, N.; Morales-Garoffolo, A.; Anderson, J. P.; Benetti, S.; Bersten, M.; Botticella, M. T.; Cappellaro, E.; Fasano, G.; Fraser, M.; Gal-Yam, A.; Gillone, M.; Graham, M. L.; Greiner, J.; Hachinger, S.; Howell, D. A.; Inserra, C.; Parrent, J.; Rau, A.; Schulze, S.; Smartt, S. J.; Smith, K. W.; Turatto, M.; Yaron, O.; Young, D. R.; Kubiak, M.; Szymanski, M. K.; Pietrzynski, G.; Soszynski, I.; Ulaczyk, K.; Poleski, R.; Pietrukowicz, P.; Skowron, J.; Mroz, P.
We present optical observations of the peculiar Type Ibn supernova (SN Ibn) OGLE-2012-SN-006, discovered and monitored by the Optical Gravitational Lensing Experiment-IV survey, and spectroscopically followed by Public ESO Spectroscopic Survey of Transient Objects (PESSTO) at late phases. Stringent pre-discovery limits constrain the explosion epoch with fair precision to JD = 245 6203.8 +/- 4.0. The rise time to the I-band light-curve maximum is about two weeks. The object reaches the peak absolute magnitude M-I = -19.65 +/- 0.19 on JD = 245 6218.1 +/- 1.8. After maximum, the light curve declines for about 25 d with a rate of 4 mag (100 d)(-1). The symmetric I-band peak resembles that of canonical Type Ib/c supernovae (SNe), whereas SNe Ibn usually exhibit asymmetric and narrower early-time light curves. Since 25 d past maximum, the light curve flattens with a decline rate slower than that of the Co-56-Fe-56 decay, although at very late phases it steepens to approach that rate. However, other observables suggest that the match with the Co-56 decay rate is a mere coincidence, and the radioactive decay is not the main mechanism powering the light curve of OGLE-2012-SN-006. An early-time spectrum is dominated by a blue continuum, with only a marginal evidence for the presence of He I lines marking this SN type. This spectrum shows broad absorptions bluewards than 5000 angstrom, likely O II lines, which are similar to spectral features observed in superluminous SNe at early epochs. The object has been spectroscopically monitored by PESSTO from 90 to 180 d after peak, and these spectra show the typical features observed in a number of SN 2006jc-like events, including a blue spectral energy distribution and prominent and narrow (v(FWHM) approximate to 1900 km s(-1)) He I emission lines. This suggests that the ejecta are interacting with He-rich circumstellar material. The detection of broad (10(4) km s(-1)) O I and Ca II features likely produced in the SN ejecta (including the [OI] lambda lambda 6300,6364 doublet in the latest spectra) lends support to the interpretation of OGLE-2012-SN-006 as a core-collapse event.
Photometric and spectroscopic evolution of the interacting transient AT 2016jbu(Gaia16cfr)
(2022) Brennan, S. J.; Fraser, M.; Johansson, J.; Pastorello, A.; Kotak, R.; Stevance, H. F.; Chen, T-W; Eldridge, J. J.; Bose, S.; Brown, P. J.; Callis, E.; Cartier, R.; Dennefeld, M.; Dong, Subo; Duffy, P.; Elias-Rosa, N.; Hosseinzadeh, G.; Hsiao, E.; Kuncarayakti, H.; Martin-Carrillo, A.; Monard, B.; Nyholm, A.; Pignata, G.; Sand, D.; Shappee, B. J.; Smartt, S. J.; Tucker, B. E.; Wyrzykowski, L.; Abbot, H.; Benetti, S.; Bento, J.; Blondin, S.; Chen, Ping; Delgado, A.; Galbany, L.; Gromadzki, M.; Gutierrez, C. P.; Hanlon, L.; Harrison, D. L.; Hiramatsu, D.; Hodgkin, S. T.; Holoien, T. W-S; Howell, D. A.; Inserra, C.; Kankare, E.; Kozlowski, S.; Muller-Bravo, T. E.; Maguire, K.; McCully, C.; Meintjes, P.; Morrell, N.; Nicholl, M.; O'Neill, D.; Pietrukowicz, P.; Poleski, R.; Prieto, J. L.; Rau, A.; Reichart, D. E.; Schweyer, T.; Shahbandeh, M.; Skowron, J.; Sollerman, J.; Soszynski, I; Stritzinger, M. D.; Szymanski, M.; Tartaglia, L.; Udalski, A.; Ulaczyk, K.; Young, D. R.; van Leeuwen, M.; van Soelen, B.
We present the results from a high-cadence, multiwavelength observation campaign of AT 2016jbu (aka Gaia16cfr), an interacting transient. This data set complements the current literature by adding higher cadence as well as extended coverage of the light-curve evolution and late-time spectroscopic evolution. Photometric coverage reveals that AT 2016jbu underwent significant photometric variability followed by two luminous events, the latter of which reached an absolute magnitude of M-V similar to-18.5 mag. This is similar to the transient SN 2009ip whose nature is still debated. Spectra are dominated by narrow emission lines and show a blue continuum during the peak of the second event. AT 2016jbu shows signatures of a complex, non-homogeneous circumstellar material (CSM). We see slowly evolving asymmetric hydrogen line profiles, with velocities of 500 km s(-)(1) seen in narrow emission features from a slow-moving CSM, and up to 10 000 km s(-1) seen in broad absorption from some high-velocity material. Late-time spectra (similar to+1 yr) show a lack of forbidden emission lines expected from a core-collapse supernova and are dominated by strong emission from H, He I, and Ca II. Strong asymmetric emission features, a bumpy light curve, and continually evolving spectra suggest an inhibit nebular phase. We compare the evolution of H alpha among SN 2009ip-like transients and find possible evidence for orientation angle effects. The light-curve evolution of AT 2016jbu suggests similar, but not identical, circumstellar environments to other SN 2009ip-like transients.
Progenitor, environment, and modelling of the interacting transient AT 2016jbu (Gaia16cfr)
(2022) Brennan, S. J.; Fraser, M.; Johansson, J.; Pastorello, A.; Kotak, R.; Stevance, H. F.; Chen, T-W; Eldridge, J. J.; Bose, S.; Brown, P. J.; Callis, E.; Cartier, R.; Dennefeld, M.; Dong, Subo; Duffy, P.; Elias-Rosa, N.; Hosseinzadeh, G.; Hsiao, E.; Kuncarayakti, H.; Martin-Carrillo, A.; Monard, B.; Pignata, G.; Sand, D.; Shappee, B. J.; Smartt, S. J.; Tucker, B. E.; Wyrzykowski, L.; Abbot, H.; Benetti, S.; Bento, J.; Blondin, S.; Chen, Ping; Delgado, A.; Galbany, L.; Gromadzki, M.; Gutierrez, C. P.; Hanlon, L.; Harrison, D. L.; Hiramatsu, D.; Hodgkin, S. T.; Holoien, T. W-S; Howell, D. A.; Inserra, C.; Kankare, E.; Kozlowski, S.; Muller-Bravo, T. E.; Maguire, K.; McCully, C.; Meintjes, P.; Morrell, N.; Nicholl, M.; O'Neill, D.; Pietrukowicz, P.; Poleski, R.; Prieto, J. L.; Rau, A.; Reichart, D. E.; Schweyer, T.; Shahbandeh, M.; Skowron, J.; Sollerman, J.; Soszynski, I; Stritzinger, M. D.; Szymanski, M.; Tartaglia, L.; Udalski, A.; Ulaczyk, K.; Young, D. R.; van Leeuwen, M.; van Soelen, B.
We present the bolometric light curve, identification and analysis of the progenitor candidate, and preliminary modelling of AT 2016jbu (Gaia16cfr). We find a progenitor consistent with a similar to 22-25 M-circle dot yellow hypergiant surrounded by a dusty circumstellar shell, in agreement with what has been previously reported. We see evidence for significant photometric variability in the progenitor, as well as strong H alpha emission consistent with pre-existing circumstellar material. The age of the environment, as well as the resolved stellar population surrounding AT 2016jbu, supports a progenitor age of >10 Myr, consistent with a progenitor mass of similar to 22 M-circle dot. A joint analysis of the velocity evolution of AT 2016jbu and the photospheric radius inferred from the bolometric light curve shows the transient is consistent with two successive outbursts/explosions. The first outburst ejected material with velocity similar to 650 km s(-1), while the second, more energetic event ejected material at similar to 4500 km s(-1). Whether the latter is the core collapse of the progenitor remains uncertain. We place a limit on the ejected Ni-56 mass of <0.016 M-circle dot. Using the Binary Population And Spectral Synthesis (BPASS) code, we explore a wide range of possible progenitor systems and find that the majority of these are in binaries, some of which are undergoing mass transfer or common-envelope evolution immediately prior to explosion. Finally, we use the SuperNova Explosion Code (SNEC) to demonstrate that the low-energy explosions within some of these binary systems, together with sufficient circumstellar material, can reproduce the overall morphology of the light curve of AT 2016jbu.
SN 2008jb: A "Lost" Core-collapse Supernova in a Star-forming Dwarf Galaxy at ~10 Mpc
(2012) Prieto, J. L.; Lee, J. C.; Drake, A. J.; McNaught, R.; Garradd, G.; Beacom, J. F.; Beshore, E.; Catelan, Marcio; Djorgovski, S. G.; Pojmanski, G.; Stanek, K. Z.; Szczygieł, D. M.
We present the discovery and follow-up observations of SN 2008jb, a core-collapse supernova in the southern dwarf irregular galaxy ESO 302-14 (MB = -15.3 mag) at 9.6 Mpc. This nearby transient was missed by galaxy-targeted surveys and was only found in archival optical images obtained by the Catalina Real-time Transient Survey and the All-Sky Automated Survey. The well-sampled archival photometry shows that SN 2008jb was detected shortly after explosion and reached a bright optical maximum, V max ~= 13.6 mag (M V, max ~= -16.5). The shape of the light curve shows a plateau of ~100 days, followed by a drop of ~1.4 mag in the V band to a slow decline with an approximate 56Co decay slope. The late-time light curve is consistent with 0.04 ± 0.01 M ⊙ of 56Ni synthesized in the explosion. A spectrum of the supernova obtained two years after explosion shows a broad, boxy Hα emission line, which is unusual for normal Type II-Plateau supernovae at late times. We detect the supernova in archival Spitzer and WISE images obtained 8-14 months after explosion, which show clear signs of warm (600-700 K) dust emission. The dwarf irregular host galaxy, ESO 302-14, has a low gas-phase oxygen abundance, 12 + log(O/H) = 8.2 (~1/5 Z ⊙), similar to those of the Small Magellanic Cloud and the hosts of long gamma-ray bursts and luminous core-collapse supernovae. This metallicity is one of the lowest among local (lsim 10 Mpc) supernova hosts. We study the host environment using GALEX far-UV, R-band, and Hα images and find that the supernova occurred in a large star formation complex. The morphology of the Hα emission appears as a large shell (R ~= 350 pc) surrounding the FUV and optical emission. Using the Hα-to-FUV ratio and FUV and R-band luminosities, we estimate an age of ~9 Myr and a total mass of ~2 × 105 M ⊙ for the star formation complex, assuming a single-age starburst. These properties are consistent with the expanding Hα supershells observed in many well-studied nearby dwarf galaxies, which are tell-tale signs of feedback from the cumulative effect of massive star winds and supernovae. The age estimated for the star-forming region where SN 2008jb exploded suggests a relatively high-mass progenitor star with an initial mass M ~ 20 M ⊙ and warrants further study. We discuss the implications of these findings in the study of core-collapse supernova progenitors. This paper includes data gathered with the 6.5 m Magellan telescope at Las Campanas Observatory, Chile....
Supernova 2010gu
(2010) McNaught, R. H.; Garradd, G.; Drake, A. J.; Djorgovski, S. G.; Mahabal, A.; Graham, M. J.; Williams, R.; Prieto, J. L.; Catelan , Marcio; Beshore, E. C.; Larson, S. M.; Christensen, E.McNaught, R. H.; Garradd, G.; Drake, A. J.; Djorgovski, S. G.; Mahabal, A.; Graham, M. J.; Williams, R.; Prieto, J. L.; Catelan , Marcio; Beshore, E. C.; Larson, S. M.; Christensen, E.McNaught, R. H.; Garradd, G.; Drake, A. J.; Djorgovski, S. G.; Mahabal, A.; Graham, M. J.; Williams, R.; Prieto, J. L.; Catelan , Marcio; Beshore, E. C.; Larson, S. M.; Christensen, E.McNaught, R. H.; Garradd, G.; Drake, A. J.; Djorgovski, S. G.; Mahabal, A.; Graham, M. J.; Williams, R.; Prieto, J. L.; Catelan , Marcio; Beshore, E. C.; Larson, S. M.; Christensen, E.McNaught, R. H.; Garradd, G.; Drake, A. J.; Djorgovski, S. G.; Mahabal, A.; Graham, M. J.; Williams, R.; Prieto, J. L.; Catelan , Marcio; Beshore, E. C.; Larson, S. M.; Christensen, E.McNaught, R. H.; Garradd, G.; Drake, A. J.; Djorgovski, S. G.; Mahabal, A.; Graham, M. J.; Williams, R.; Prieto, J. L.; Catelan , Marcio; Beshore, E. C.; Larson, S. M.; Christensen, E.McNaught, R. H.; Garradd, G.; Drake, A. J.; Djorgovski, S. G.; Mahabal, A.; Graham, M. J.; Williams, R.; Prieto, J. L.; Catelan , Marcio; Beshore, E. C.; Larson, S. M.; Christensen, E.
Further to CBET 2387, R. H. McNaught and G. Garradd, Australian National University; A. J. Drake, S. G. Djorgovski, A. Mahabal, M. J. Graham, and R. Williams, California Institute of Technology; J. L. Prieto, Carnegie Observatories; M. Catelan, Pontificia Universidad Catolica de Chile; E. C. Beshore and S. M. Larson, Lunar and Planetary Laboratory, University of Arizona; and E. Christensen, Gemini Observatory, report the CRTS discovery of an apparent supernova in unfiltered Siding Spring Survey (SSS) images: SN 2010 UT R.A. (2000.0) Decl. Mag. Offset 2010gu Aug. 7.67 22 19 23.16 -36 58 24.5 18.0 7".0 E, 3".3 N Further SSS magnitudes for 2010gu: July 9.81, [19.5; Aug. 10.76, 17.9. The host galaxy, 2MASX J22192259-3658278, has redshift z = 0.056....
Supernova 2010hj in Pgc 67413
(2010) Drake, A. J.; Djorgovski, S. G.; Mahabal, A.; Graham, M. J.; Williams, R.; McNaught, R. H.; Garradd, G.; Howerton, S.; Prieto, J. L.; Catelan , Marcio; Beshore, E. C.; Larson, S. M.; Christensen, E.
Report the discovery of an apparent supernova in unfiltered Siding Spring Survey (SSS) images: SN 2010 UT R.A. (2000.0) Decl. Mag. Offset 2010hj Aug. 4.61 21 49 09.84 -59 02 23.2 17.1 5".5 W, 8".2 S Nothing was visible at this position on an SSS image from 2009 Oct. 1.50 UT (limitiing mag 18.9), but 2010hj was detected again in SSS images on Aug. 29.59 (no magnitude provided). The host galaxy appears to be PGC 67413 = ESO 145-G16. Joseph Brimacombe, Cairns, Australia, reports that ten stacked 600-s CCD images (limiting magnitude 20) taken remotely with a 32-cm RCOS telescope (+ STL6K camera + clear filter) at the Macedon Ranges Observatory near Melbourne, Australia, on Aug. 29.727 show the new object to be at mag 18.3 and located approximately 7" west and 7" south of the presumed host-galaxy nucleus. Another stacked image (seven 1200-s frames; limiting magnitude 20), taken by Brimacombe on Sept. 2.636 with a 40-cm RCOS telescope (+ U16 camera + red filter) at the Coral Towers Observatory (Cairns), yields mag 18.6 for 2010hj; the Sept. 2 stacked image has been posted at the following website URL: http://www.flickr.com/photos/43846774@N02/4952444311/....
Supernova 2010iw near UGC 4570
(2010) Howerton, C.; Drake, A. J.; Djorgovski, S. G.; Mahabal, A.; Graham, M. J.; Williams, R.; Prieto, J. L.; Catelan , Marcio; Beshore, E. C.; Larson, S. M.; Christensen, E.
Report the discovery by Howerton of an apparent supernova in public Catalina Sky Survey (CSS) images: SN 2010 UT R.A. (2000.0) Decl. Mag. Offset 2010iw Oct. 14.66 8 45 15.01 +27 49 21.8 16.4 12".9 W, 3".4 S Further magnitudes for 2010iw: June 11.16 UT, [19.0 (CSS); Oct. 17.50, 16.3 (Howerton, remotely with a 0.6-m LB-1 telescope, Rodeo, NM, U.S.A.). They note that the new object lies 5".4 east and 1".1 north from a galaxy seen in Sloan Digital Sky Survey images with measured redshift z = 0.109; the current luminosity of 2010iw appears too high for it to be a regular supernova associated with this distant galaxy. The host galaxy is thus is likely to be UGC 4570 (at redshift z = 0.0215)....
Supernova 2010jt
(2010) Howerton, S.; Drake, A. J.; Djorgovski, S. G.; Mahabal, A.; Graham, M. J.; Williams, R.; McNaught, R. H.; Garradd, G.; Prieto, J. L.; Catelan , Marcio; Beshore, E. C.; Larson, S. M.; Christensen, E.
Report the discovery of an apparent supernova in Siding Spring Survey (SSS) images made public via the "Catalina Real-time Transient Survey" program: SN 2010 UT R.A. (2000.0) Decl. Mag. Offset 2010jt Nov. 6.57 23 43 41.24 -41 18 46.9 19.0 20".5 E, 29".6 N Further SSS magnitudes for 2010jt: Oct. 18.51 UT, [20.5 (co-added image); Nov. 7.50, 19.0. The likely host galaxy, 6dFGS gJ234339.4-411917, has redshift z = 0.053....
Supernova 2010kq in UGC 1769
(2010) Howerton, S.; Drake, A. J.; Djorgovski, S. G.; Mahabal, A.; Graham, M. J.; Williams, R.; Prieto, J. L.; Catelan , Marcio; Beshore, E. C.; Larson, S. M.; Christensen, E.
Report the CRTS discovery of an apparent supernova in public images from the Catalina Sky Survey (CSS). SN 2010 UT R.A. (2000.0) Decl. Mag. Offset 2010kq Dec. 7.23 2 18 10.92 +37 05 42.4 18.3 0".3 E, 4".9 S After posting on the CBAT's unconfirmed-objects webpage, Markku Nissinen and Veli-Pekka Hentunen (Varkaus, Finland) report that their exposures (limiting mag R = 18.9; 3-sigma) taken on Dec. 9 remotely with a 51-cm f/6.8 GRAS011 Global-Rent-a-Scope (+ FLI ProLine PL-11002M camera) near Mayhill, NM, USA, yield position end figures 11s.05, 39".9 for 2010kq (which is 1".5 east and 6".1 south of the center of the galaxy UGC 1769); they note that nothing is visible at this position on a red Palomar Sky Survey F plate. Further CCD magnitude estimates for 2010kq (unfiltered unless otherwise noted): Nov. 15.20 UT, [19.5 (CSS); Dec. 9.088, R = 16.4 +/- 0.1 (Nissinen and Hentunen); 9.14, 16.4 (Howerton; remotely using the LB-1 0.6m telescope at Rodeo, NM, U.S.A.). Drake notes that the presumed host galaxy, UGC 1769, has redshift z = 0.027....
Supernova 2010ks in UGC 5622
(2010) Howerton, S.; Drake, A. J.; Djorgovski, S. G.; Mahabal, A.; Graham, M. J.; Williams, R.; Prieto, J. L.; Catelan , Marcio; Beshore, E. C.; Larson, S. M.; Christensen, E.
Report the CRTS discovery of an apparent supernova in public images from Catalina Sky Survey (CSS). SN 2010 UT R.A. (2000.0) Decl. Mag. Offset 2010ks Dec. 11.46 10 23 42.44 +33 46 49.0 17.0 7".8 E, 22".0 N Further unfiltered CCD magnitude estimates of 2010ks: June 15.20 UT, [19.3 (CSS); Dec. 12.42, 17.4 (LB-1 0.6-m telescope at Rodeo, NM). The presumed host galaxy, UGC 5622, has redshift z = 0.033....
Supernova 2010ll
(2010) Drake, A. J.; Djorgovski, S. G.; Mahabal, A.; Graham, M. J.; Williams, R.; Prieto, J. L.; Catelan , Marcio; Beshore, E. C.; Larson, S. M.; Christensen, E.
Report the CRTS discovery of an apparent supernova in unfiltered Catalina Sky Survey (CSS) images: SN 2010 UT R.A. (2000.0) Decl. Mag. Offset 2010ll Dec. 10.32 4 50 29.81 -10 44 17.0 18.1 11".8 W, 6".3 N Further CSS magnitudes for 2010ll: Nov. 16.39 UT, [20.4; Nov. 30.35, 19.0....
Supernova 2010lr
(2011) Drake, A. J.; Djorgovski, S. G.; Mahabal, A.; Graham, M. J.; Williams, R.; McNaught, R. H.; Garradd, G.; Prieto, J. L.; Catelan , Marcio; Beshore, E. C.; Larson, S. M.; Christensen, E.
Report the CRTS discovery of an apparent supernova in unfiltered Siding Spring Survey (SSS) images: SN 2010 UT R.A. (2000.0) Decl. Mag. Offset 2010lr Dec. 30.46 0 02 35.50 -30 43 52.4 18.0 19".4 E, 13".3 N Further SSS magnitudes for 2010lr: 2010 Nov. 4.58 UT, [20.1; Dec. 28.47, 17.9. The presumed host galaxy, 2MASX J00023401-3044061, has redshift z = 0.062....
Supernova 2010lu
(2011) Drake, A. J.; Djorgovski, S. G.; Mahabal, A.; Graham, M. J.; Williams, R.; Prieto, J. L.; Catelan , Marcio; Beshore, E. C.; Larson, S. M.; Christensen, E.
Report the CRTS discovery of an apparent supernova in unfiltered Catalina Sky Survey (CSS) images: SN 2010 UT R.A. (2000.0) Decl. Mag. Offset 2010lu Dec. 8.40 9 06 00.70 +29 20 32.5 16.8 5".8 E, 8".3 S Further CSS magnitudes for 2010lu: 2010 Nov. 7.51 UT, [19.5; 2011 Jan. 3.34, 17.1. The presumed host galaxy, SDSS J090600.26+292041.0, has redshift z = 0.023....
Supernova 2011ae in MCG -03-30-19 = Psn J11544925-1651436
(2011) Howerton, S.; Drake, A. J.; Djorgovski, S. G.; Mahabal, A.; Graham, M. J.; Williams, R.; Prieto, J. L.; Catelan , Marcio; Beshore, E. C.; Larson, S. M.; Christensen, E.; Sahu, D. K.; Arora, S.; Anto, P.
Report the Catalina Real-time Transient Survey's discovery of an apparent supernova in public images from the Catalina Sky Survey (CSS). SN 2011 UT R.A. (2000.0) Decl. Mag. Offset 2011ae Feb. 12.43 11 54 49.25 -16 51 43.6 15.5 4".9 W, 8".4 N Further unfiltered CCD magnitude estimates for 2011ae: Feb. 5.46 UT, [18.5 (CSS); 13.41, 15.3 (remotely with the LB3 0.35-m telescope at Rodeo, NM, U.S.A.). Drake writes that the presumed host galaxy has redshift z = 0.0060. The object was given the designation PSN J11544925-1651436 when posted by Drake on the Central Bureau's TOCP webpage, and based on the spectroscopy below is here assigned the final designation SN 2011ae. D. K. Sahu, S. Arora, and P. Anto, Indian Institute of Astrophysics, Bangalore, report that a low-resolution spectrogram (range 350-930 nm) of 2011ae, obtained on Feb. 21.75 UT with the Indian Astronomical Observatory's 2-m Himalayan Chandra Telescope (+ HFOSC), shows it to be a normal type-Ia supernova, a few days before maximum light. Using the SNID code of Blondin and Tonry (2007, Ap.J. 666, 1024), the spectrum of 2011ae is found to best match that of SN 1990N at about 5 days before maximum light. Adopting a recession velocity of 1813 km/s for the presumed host galaxy (de Vaucouleurs et al. 1991, Third Reference Catalogue of Bright Galaxies), MCG -03-30-19, the velocity corresponding to the Si II 635.5-nm absorption line is 12500 km/s....
Supernova 2011af = Psn J02255436+1023111
(2011) Drake, A. J.; Djorgovski, S. G.; Mahabal, A.; Graham, M. J.; Williams, R.; Prieto, J. L.; Catelan , Marcio; Beshore, E. C.; Larson, S. M.; Christensen, E.; Hsiao, E. Y.
Report the Catalina Real-time Transient Survey's discovery of an apparent supernova in unfiltered Catalina Sky Survey (CSS) images: SN 2011 UT R.A. (2000.0) Decl. Mag. Offset 2011af Jan. 11.09 2 25 54.36 +10 23 11.1 16.7 4" W, 1" N Further CSS magnitude estimates for 2011af: 2010 Dec. 10.21 UT, [19.0; 2011 Jan. 5.15, 16.5. This object was designated PSN J02255436+1023111 when posted at the Central Bureau's TOCP webpage by Drake, and based on the spectroscopy below is here designated SN 2011af. Kuiyun Huang and Yoichi Ohyama, Institute of Astronomy and Astrophysics, Academia Sinica; Chia-Jung Chuang, Yuji Urata, and Induk Lee, National Central University, Taiwan; and Eric Y. Hsiao, Lawrence Berkeley National Laboratory, report that the inspection of a CCD spectrum (range 400-900 nm), obtained on Jan. 29.5 UT with the 1.8-m Ritchey Cretien reflector and medium dispersion spectrometer at Bohyunsan Optical Astronomy Observatory, Korea, shows that SN 2011af is a type-IIn supernova. The spectrum consists of a flat continuum and prominent narrow emission lines of the Balmer series (H-alpha FWHM of about 1500 km/s), with the narrow peaks yielding a redshift of 0.064. The "superfit" program of Howell et al. (2005, Ap.J. 634, 1190) shows its spectrum to be an excellent match to that of SN 1988Z. SN 2011af is measured to have a magnitude r' about 17.2 on Feb. 7.46 UT with the 1-m telescope at the Lulin Observatory in Taiwan; this corresponds to an absolute magnitude of about -20, nearly a month past its initial discovery....
Supernova 2011ag in Pgc 11943 = Psn J03122655+1915064
(2011) Drake, A. J.; Djorgovski, S. G.; Mahabal, A.; Graham, M. J.; Williams, R.; Prieto, J. L.; Catelan , Marcio; Beshore, E. C.; Larson, S. M.; Christensen, E.; Koff, R. A.; Hsiao, E. Y.; Suzuki, N.; Nugent, P. E.
Report the Catalina Real-time Transient Survey's discovery of an apparent supernova in unfiltered Catalina Sky Survey (CSS) images: SN 2011 UT R.A. (2000.0) Decl. Mag. Offset 2011ag Feb. 25.15 3 12 26.55 +19 15 06.4 17.3 3".5 E, 20".0 N This object was designated PSN J03122655+1915064 on the Central Bureau's TOCP webpage, and is here designated SN 2011ag based on the spectroscopic report below. Further unfiltered CCD magnitudes for 2011ag: Feb. 4.11 UT, [20.4 (CSS); 27.089, 17.7 (R. A. Koff, Bennett, CO, U.S.A.; fourteen co-added 60-s images; position end figures 26s.55, 05".1). E. Y. Hsiao, N. Suzuki, and P. E. Nugent, Lawrence Berkeley National Laboratory, report that inspection of a CCD spectrum (range 350-980 nm), obtained on Feb. 27.25 UT with the 3-m Shane reflector (+ Kast) at Lick Observatory, shows that 2011ag is a type-Ia supernova. The "superfit" software of Howell et al. (2005, Ap.J. 634, 1190) identified the spectrum as that of a type-Ia supernova around a week past maximum. The redshift matches that of the reported host galaxy (PGC 11943): z = 0.032. The spectrum closely resembles that of SN 1998bu at 10 days past maximum (Jha et al. 1999, Ap.J. Suppl. 125, 73)....

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