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1. The HST See Change Program. I. Survey Design, Pipeline, and Supernova Discoveries

Author: Hayden, Brian, Rubin, David, Boone, Kyle, Aldering, Greg, Nordin, Jakob, Brodwin, Mark, Deustua, Susana, Dixon, Sam, Fagrelius, Parker, Fruchter, Andy, Eisenhardt, Peter, Gonzalez, Anthony, Gupta, Ravi, Hook, Isobel, Lidman, Chris, Luther, Kyle, Muzzin, Adam, Raha, Zachary, Ruiz-Lapuente, Pilar, Saunders, Clare, Sofiatti, Caroline, Stanford, Adam, Suzuki, Nao, Webb, Tracy, Williams, Steven C., Wilson, Gillian, Yen, Mike, Amanullah, Rahman, Barbary, Kyle, Böhringer, Hans, Chappell, Greta, Cunha, Carlos, Currie, Miles, Fassbender, Rene, Gladders, Michael, Goobar, Ariel, Hildebrandt, Hendrik, Hoekstra, Henk, Huang, Xiaosheng, Huterer, Dragan, Jee, M. James, Kim, Alex, Kowalski, Marek, Linder, Eric, Meyers, Joshua E., Pain, Reynald, Perlmutter, Saul, Richard, Johan, Rosati, Piero, Rozo, Eduardo, Rykoff, Eli, Santos, Joana, Spadafora, Anthony, Stern, Daniel, Wechsler, Risa, Hayden, Brian, Rubin, David, Boone, Kyle, Aldering, Greg, Nordin, Jakob, Brodwin, Mark, Deustua, Susana, Dixon, Sam, Fagrelius, Parker, Fruchter, Andy, Eisenhardt, Peter, Gonzalez, Anthony, Gupta, Ravi, Hook, Isobel, Lidman, Chris, Luther, Kyle, Muzzin, Adam, Raha, Zachary, Ruiz-Lapuente, Pilar, Saunders, Clare, Sofiatti, Caroline, Stanford, Adam, Suzuki, Nao, Webb, Tracy, Williams, Steven C., Wilson, Gillian, Yen, Mike, Amanullah, Rahman, Barbary, Kyle, Böhringer, Hans, Chappell, Greta, Cunha, Carlos, Currie, Miles, Fassbender, Rene, Gladders, Michael, Goobar, Ariel, Hildebrandt, Hendrik, Hoekstra, Henk, Huang, Xiaosheng, Huterer, Dragan, Jee, M. James, Kim, Alex, Kowalski, Marek, Linder, Eric, Meyers, Joshua E., Pain, Reynald, Perlmutter, Saul, Richard, Johan, Rosati, Piero, Rozo, Eduardo, Rykoff, Eli, Santos, Joana, Spadafora, Anthony, Stern, Daniel, and Wechsler, Risa
Abstract: The See Change survey was designed to make z > 1 cosmological measurements by efficiently discovering high-redshift Type Ia supernovae (SNe Ia) and improving cluster mass measurements through weak lensing. This survey observed twelve galaxy clusters with the Hubble Space Telescope (HST) spanning the redshift range z = 1.13-1.75, discovering 57 likely transients and 27 likely SNe Ia at z similar to 0.8-2.3. As in similar previous surveys, this proved to be a highly efficient use of HST for supernova observations; the See Change survey additionally tested the feasibility of maintaining, or further increasing, the efficiency at yet higher redshifts, where we have less detailed information on the expected cluster masses and star formation rates. We find that the resulting number of SNe Ia per orbit is a factor of similar to 8 higher than for a field search, and 45% of our orbits contained an active SN Ia within 22 rest-frame days of peak, with one of the clusters by itself yielding 6 of the SNe Ia. We present the survey design, pipeline, and supernova discoveries. Novel features include fully blinded supernova searches, the first random forest candidate classifier for undersampled IR data (with a 50% detection threshold within 0.05 mag of human searchers), real-time forward-modeling photometry of candidates, and semi-automated photometric classifications and follow-up forecasts. We also describe the spectroscopic follow-up, instrumental in measuring host galaxy redshifts. The cosmology analysis of our sample will be presented in a companion paper.
Published: 2021
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2. The HST See Change Program: I. Survey Design, Pipeline, and Supernova Discoveries

Author: Hayden, Brian, Rubin, David, Boone, Kyle, Aldering, Greg, Nordin, Jakob, Brodwin, Mark, Deustua, Susana, Dixon, Sam, Fagrelius, Parker, Fruchter, Andy, Eisenhardt, Peter, Gonzalez, Anthony, Gupta, Ravi, Hook, Isobel, Lidman, Chris, Luther, Kyle, Muzzin, Adam, Raha, Zachary, Ruiz-Lapuente, Pilar, Saunders, Clare, Sofiatti, Caroline, Stanford, Adam, Suzuki, Nao, Webb, Tracy, Williams, Steven C., Wilson, Gillian, Yen, Mike, Amanullah, Rahman, Barbary, Kyle, Bohringer, Hans, Chappell, Greta, Cunha, Carlos, Currie, Miles, Fassbender, Rene, Gladders, Michael, Goobar, Ariel, Hildenrandt, Hendrik, Hoekstra, Henk, Huang, Xiaosheng, Huterer, Dragan, Jee, M. James, Kim, Alex, Kowalski, Marek, Linder, Eric, Meyers, Joshua E., Pain, Reynald, Perlmutter, Saul, Richard, Johan, Rosati, Piero, Rozo, Eduardo, Rykoff, Eli, Santos, Joana, Spadafora, Anthony, Stern, Daniel, Wechsler, Risa, Project, The Supernova Cosmology, Hayden, Brian, Rubin, David, Boone, Kyle, Aldering, Greg, Nordin, Jakob, Brodwin, Mark, Deustua, Susana, Dixon, Sam, Fagrelius, Parker, Fruchter, Andy, Eisenhardt, Peter, Gonzalez, Anthony, Gupta, Ravi, Hook, Isobel, Lidman, Chris, Luther, Kyle, Muzzin, Adam, Raha, Zachary, Ruiz-Lapuente, Pilar, Saunders, Clare, Sofiatti, Caroline, Stanford, Adam, Suzuki, Nao, Webb, Tracy, Williams, Steven C., Wilson, Gillian, Yen, Mike, Amanullah, Rahman, Barbary, Kyle, Bohringer, Hans, Chappell, Greta, Cunha, Carlos, Currie, Miles, Fassbender, Rene, Gladders, Michael, Goobar, Ariel, Hildenrandt, Hendrik, Hoekstra, Henk, Huang, Xiaosheng, Huterer, Dragan, Jee, M. James, Kim, Alex, Kowalski, Marek, Linder, Eric, Meyers, Joshua E., Pain, Reynald, Perlmutter, Saul, Richard, Johan, Rosati, Piero, Rozo, Eduardo, Rykoff, Eli, Santos, Joana, Spadafora, Anthony, Stern, Daniel, Wechsler, Risa, and Project, The Supernova Cosmology
Abstract: The See Change survey was designed to make $z>1$ cosmological measurements by efficiently discovering high-redshift Type Ia supernovae (SNe Ia) and improving cluster mass measurements through weak lensing. This survey observed twelve galaxy clusters with the Hubble Space Telescope spanning the redshift range $z=1.13$ to $1.75$, discovering 57 likely transients and 27 likely SNe Ia at $z\sim 0.8-2.3$. As in similar previous surveys (Dawson et al. 2009), this proved to be a highly efficient use of HST for SN observations; the See Change survey additionally tested the feasibility of maintaining, or further increasing, the efficiency at yet higher redshifts, where we have less detailed information on the expected cluster masses and star-formation rates. We find that the resulting number of SNe Ia per orbit is a factor of $\sim 8$ higher than for a field search, and 45% of our orbits contained an active SN Ia within 22 rest-frame days of peak, with one of the clusters by itself yielding 6 of the SNe Ia. We present the survey design, pipeline, and SN discoveries. Novel features include fully blinded SN searches, the first random forest candidate classifier for undersampled IR data (with a 50% detection threshold within 0.05 magnitudes of human searchers), real-time forward-modeling photometry of candidates, and semi-automated photometric classifications and follow-up forecasts. We also describe the spectroscopic follow-up, instrumental in measuring host-galaxy redshifts. The cosmology analysis of our sample will be presented in a companion paper., Comment: ApJ preprint
Published: 2021
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3. The HST See Change Program. I. Survey Design, Pipeline, and Supernova Discoveries

Author: Gemini Observatory, National Science Foundation (US), National Research Council of Canada, Comisión Nacional de Investigación Científica y Tecnológica (Chile), Ministerio de Ciencia, Tecnología e Innovación Productiva (Argentina), Ministério da Ciência, Tecnologia e Inovação (Brasil), Korea Astronomy and Space Science Institute, European Southern Observatory, National Aeronautics and Space Administration (US), German Research Foundation, European Commission, Hayden, Brian, Rubin, David, Boone, Kyle, Aldering, Greg, Nordin, Jakob, Brodwin, Mark, Deustua, Susana, Dixon, Sam, Fagrelius, Parker, Fruchter, Andrew S., Eisenhardt, Peter, Gonzalez, Anthony, Gupta, Ravi, Hook, Isobel, Lidman, Chris, Luther, Kyle, Muzzin, Adam, Raha, Zachary, Ruiz-Lapuente, Pilar, Saunders, Clare, Sofiatti, Caroline, Stanford, Adam, Suzuki, Nao, Webb, Tracy, Williams, Steven C., Wilson, Gillian, Yen, Mike, Amanullah, Rahman, Barbary, Kyle, Böhringer, Hans, Chappell, Greta, Cunha, Carlos, Currie, Miles, Fassbender, Rene, Gladders, Michael, Goobar, Ariel, Hildebrandt, Hendrik, Hoekstra, Henk, Huang, Xiaosheng, Huterer, Dragan, Jee, M. James, Kim, Alex, Kowalski, Marek, Linder, Eric, Meyers, Joshua E., Pain, Reynald, Perlmutter, Saul, Richard, Johan, Rosati, Piero, Rozo, Eduardo, Rykoff, Eli, Santos, Joana, Spadafora, Anthony, Stern, Daniel, Wechsler, Risa, Gemini Observatory, National Science Foundation (US), National Research Council of Canada, Comisión Nacional de Investigación Científica y Tecnológica (Chile), Ministerio de Ciencia, Tecnología e Innovación Productiva (Argentina), Ministério da Ciência, Tecnologia e Inovação (Brasil), Korea Astronomy and Space Science Institute, European Southern Observatory, National Aeronautics and Space Administration (US), German Research Foundation, European Commission, Hayden, Brian, Rubin, David, Boone, Kyle, Aldering, Greg, Nordin, Jakob, Brodwin, Mark, Deustua, Susana, Dixon, Sam, Fagrelius, Parker, Fruchter, Andrew S., Eisenhardt, Peter, Gonzalez, Anthony, Gupta, Ravi, Hook, Isobel, Lidman, Chris, Luther, Kyle, Muzzin, Adam, Raha, Zachary, Ruiz-Lapuente, Pilar, Saunders, Clare, Sofiatti, Caroline, Stanford, Adam, Suzuki, Nao, Webb, Tracy, Williams, Steven C., Wilson, Gillian, Yen, Mike, Amanullah, Rahman, Barbary, Kyle, Böhringer, Hans, Chappell, Greta, Cunha, Carlos, Currie, Miles, Fassbender, Rene, Gladders, Michael, Goobar, Ariel, Hildebrandt, Hendrik, Hoekstra, Henk, Huang, Xiaosheng, Huterer, Dragan, Jee, M. James, Kim, Alex, Kowalski, Marek, Linder, Eric, Meyers, Joshua E., Pain, Reynald, Perlmutter, Saul, Richard, Johan, Rosati, Piero, Rozo, Eduardo, Rykoff, Eli, Santos, Joana, Spadafora, Anthony, Stern, Daniel, and Wechsler, Risa
Abstract: The See Change survey was designed to make z > 1 cosmological measurements by efficiently discovering high-redshift Type Ia supernovae (SNe Ia) and improving cluster mass measurements through weak lensing. This survey observed twelve galaxy clusters with the Hubble Space Telescope (HST) spanning the redshift range z = 1.13-1.75, discovering 57 likely transients and 27 likely SNe Ia at z ~ 0.8-2.3. As in similar previous surveys, this proved to be a highly efficient use of HST for supernova observations; the See Change survey additionally tested the feasibility of maintaining, or further increasing, the efficiency at yet higher redshifts, where we have less detailed information on the expected cluster masses and star formation rates. We find that the resulting number of SNe Ia per orbit is a factor of ~8 higher than for a field search, and 45% of our orbits contained an active SN Ia within 22 rest-frame days of peak, with one of the clusters by itself yielding 6 of the SNe Ia. We present the survey design, pipeline, and supernova discoveries. Novel features include fully blinded supernova searches, the first random forest candidate classifier for undersampled IR data (with a 50% detection threshold within 0.05 mag of human searchers), real-time forward-modeling photometry of candidates, and semi-automated photometric classifications and follow-up forecasts. We also describe the spectroscopic follow-up, instrumental in measuring host galaxy redshifts. The cosmology analysis of our sample will be presented in a companion paper. * Based on observations with the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science Institute, which is operated by AURA, Inc., under NASA contract NAS 5-26555, under programs 13677, 14327.
Published: 2021

4. High-Redshift SNe with Subaru and HST

Author: Rubin, David, Suzuki, Nao, Regnault, Nicolas, Saunders, Clare M., Currie, Miles, Han, Jesse, Aldering, Greg, Amanullah, Rahman, Antilogus, Pierre, Astier, Pierre, Barbary, Kyle, Betoule, Marc, Boone, Kyle R., Deustua, Susana, Doi, Mamoru, Fruchter, Andrew S., Goobar, Ariel, Hayden, Brian, Hazenberg, Francois, Hook, Isobel, Huang, Xiaosheng, Jiang, Jian, Kato, Takahiro, Kim, Alex, Kowalski, Marek, Lidman, Chris, Linder, Eric, Maeda, Keiichi, Morokuma, Tomoki, Nordin, Jakob, Pain, Reynald, Perlmutter, Saul, Ruiz-Lapuente, Pilar, Sako, Masao, Spadafora, Anthony, Tanaka, Masaomi, Tominaga, Nozomu, Yasuda, Naoki, Yoshida, Naoki, Rubin, David, Suzuki, Nao, Regnault, Nicolas, Saunders, Clare M., Currie, Miles, Han, Jesse, Aldering, Greg, Amanullah, Rahman, Antilogus, Pierre, Astier, Pierre, Barbary, Kyle, Betoule, Marc, Boone, Kyle R., Deustua, Susana, Doi, Mamoru, Fruchter, Andrew S., Goobar, Ariel, Hayden, Brian, Hazenberg, Francois, Hook, Isobel, Huang, Xiaosheng, Jiang, Jian, Kato, Takahiro, Kim, Alex, Kowalski, Marek, Lidman, Chris, Linder, Eric, Maeda, Keiichi, Morokuma, Tomoki, Nordin, Jakob, Pain, Reynald, Perlmutter, Saul, Ruiz-Lapuente, Pilar, Sako, Masao, Spadafora, Anthony, Tanaka, Masaomi, Tominaga, Nozomu, Yasuda, Naoki, and Yoshida, Naoki
Abstract: High-redshift type Ia supernovae are crucial for constraining any time variation in dark energy. Here, we present the first discoveries and light curves from the SUbaru Supernovae with Hubble Infrared (SUSHI) program, which combines high-redshift SN discoveries from the Subaru Strategic Program (SSP, as well as other Subaru time) with HST WFC3 IR followup. This program efficiently uses the wide field and high collecting area of Subaru Hyper Suprime-Cam for optical light curves, but still obtains a precision NIR color. We are on track to double the number of well-measured SNe Ia at z > 1.1, triggering on 23 SNe Ia in our first season.
Published: 2019

5. The Discovery of a Gravitationally Lensed Supernova Ia at Redshift 2.22

Author: Rubin, David, Hayden, Brian, Huang, Xiaosheng, Aldering, Greg, Amanullah, Rahman, Barbary, Kyle, Boone, Kyle, Brodwin, Mark, Deustua, Susana E., Dixon, Sam, Eisenhardt, Peter, Fruchter, Andrew S., Gonzalez, Anthony H., Goobar, Ariel, Gupta, Ravi R., Hook, Isobel, Jee, M. James, Kim, Alex G., Kowalski, Marek, Lidman, Chris E., Linder, Eric, Luther, Kyle, Nordin, Jakob, Pain, Reynald, Perlmutter, Saul, Raha, Zachary, Rigault, Mickael, Ruiz-Lapuente, Pilar, Saunders, Clare M., Sofiatti, Caroline, Spadafora, Anthony L., Stanford, S. Adam, Stern, Daniel, Suzuki, Nao, Williams, Steven C., Rubin, David, Hayden, Brian, Huang, Xiaosheng, Aldering, Greg, Amanullah, Rahman, Barbary, Kyle, Boone, Kyle, Brodwin, Mark, Deustua, Susana E., Dixon, Sam, Eisenhardt, Peter, Fruchter, Andrew S., Gonzalez, Anthony H., Goobar, Ariel, Gupta, Ravi R., Hook, Isobel, Jee, M. James, Kim, Alex G., Kowalski, Marek, Lidman, Chris E., Linder, Eric, Luther, Kyle, Nordin, Jakob, Pain, Reynald, Perlmutter, Saul, Raha, Zachary, Rigault, Mickael, Ruiz-Lapuente, Pilar, Saunders, Clare M., Sofiatti, Caroline, Spadafora, Anthony L., Stanford, S. Adam, Stern, Daniel, Suzuki, Nao, and Williams, Steven C.
Abstract: We present the discovery and measurements of a gravitationally lensed supernova (SN) behind the galaxy cluster MOO J1014+0038. Based on multi-band Hubble Space Telescope and Very Large Telescope (VLT) photometry of the supernova, and VLT spectroscopy of the host galaxy, we find a 97.5% probability that this SN is a SN Ia, and a 2.5% chance of a CC SN. Our typing algorithm combines the shape and color of the light curve with the expected rates of each SN type in the host galaxy. With a redshift of 2.2216, this is the highest redshift SN Ia discovered with a spectroscopic host-galaxy redshift. A further distinguishing feature is that the lensing cluster, at redshift 1.23, is the most distant to date to have an amplified SN. The SN lies in the middle of the color and light-curve shape distributions found at lower redshift, disfavoring strong evolution to z = 2.22. We estimate an amplification due to gravitational lensing of 2.8+0.6-0.5 (1.10 +- 0.23 mag)---compatible with the value estimated from the weak-lensing-derived mass and the mass-concentration relation from LambdaCDM simulations---making it the most amplified SN Ia discovered behind a galaxy cluster.
Published: 2018

6. The Discovery of a Gravitationally Lensed Supernova Ia at Redshift 2.22

Author: Rubin, David, Hayden, Brian, Huang, Xiaosheng, Aldering, Greg, Amanullah, Rahman, Barbary, Kyle, Boone, Kyle, Brodwin, Mark, Deustua, Susana E., Dixon, Sam, Eisenhardt, Peter, Fruchter, Andrew S., Gonzalez, Anthony H., Goobar, Ariel, Gupta, Ravi R., Hook, Isobel, Jee, M. James, Kim, Alex G., Kowalski, Marek, Lidman, Chris E., Linder, Eric, Luther, Kyle, Nordin, Jakob, Pain, Reynald, Perlmutter, Saul, Raha, Zachary, Rigault, Mickael, Ruiz-Lapuente, Pilar, Saunders, Clare M., Sofiatti, Caroline, Spadafora, Anthony L., Stanford, S. Adam, Stern, Daniel, Suzuki, Nao, Williams, Steven C., Rubin, David, Hayden, Brian, Huang, Xiaosheng, Aldering, Greg, Amanullah, Rahman, Barbary, Kyle, Boone, Kyle, Brodwin, Mark, Deustua, Susana E., Dixon, Sam, Eisenhardt, Peter, Fruchter, Andrew S., Gonzalez, Anthony H., Goobar, Ariel, Gupta, Ravi R., Hook, Isobel, Jee, M. James, Kim, Alex G., Kowalski, Marek, Lidman, Chris E., Linder, Eric, Luther, Kyle, Nordin, Jakob, Pain, Reynald, Perlmutter, Saul, Raha, Zachary, Rigault, Mickael, Ruiz-Lapuente, Pilar, Saunders, Clare M., Sofiatti, Caroline, Spadafora, Anthony L., Stanford, S. Adam, Stern, Daniel, Suzuki, Nao, and Williams, Steven C.
Abstract: We present the discovery and measurements of a gravitationally lensed supernova (SN) behind the galaxy cluster MOO J1014+0038. Based on multi-band Hubble Space Telescope and Very Large Telescope (VLT) photometry of the supernova, and VLT spectroscopy of the host galaxy, we find a 97.5% probability that this SN is a SN Ia, and a 2.5% chance of a CC SN. Our typing algorithm combines the shape and color of the light curve with the expected rates of each SN type in the host galaxy. With a redshift of 2.2216, this is the highest redshift SN Ia discovered with a spectroscopic host-galaxy redshift. A further distinguishing feature is that the lensing cluster, at redshift 1.23, is the most distant to date to have an amplified SN. The SN lies in the middle of the color and light-curve shape distributions found at lower redshift, disfavoring strong evolution to z = 2.22. We estimate an amplification due to gravitational lensing of 2.8+0.6-0.5 (1.10 +- 0.23 mag)---compatible with the value estimated from the weak-lensing-derived mass and the mass-concentration relation from LambdaCDM simulations---making it the most amplified SN Ia discovered behind a galaxy cluster.
Published: 2018

7. The Discovery of a Gravitationally Lensed Supernova Ia at Redshift 2.22

Author: Rubin, David, Hayden, Brian, Huang, Xiaosheng, Aldering, Greg, Amanullah, Rahman, Barbary, Kyle, Boone, Kyle, Brodwin, Mark, Deustua, Susana E., Dixon, Sam, Eisenhardt, Peter, Fruchter, Andrew S., Gonzalez, Anthony H., Goobar, Ariel, Gupta, Ravi R., Hook, Isobel, Jee, M. James, Kim, Alex G., Kowalski, Marek, Lidman, Chris E., Linder, Eric, Luther, Kyle, Nordin, Jakob, Pain, Reynald, Perlmutter, Saul, Raha, Zachary, Rigault, Mickael, Ruiz-Lapuente, Pilar, Saunders, Clare M., Sofiatti, Caroline, Spadafora, Anthony L., Stanford, S. Adam, Stern, Daniel, Suzuki, Nao, Williams, Steven C., Rubin, David, Hayden, Brian, Huang, Xiaosheng, Aldering, Greg, Amanullah, Rahman, Barbary, Kyle, Boone, Kyle, Brodwin, Mark, Deustua, Susana E., Dixon, Sam, Eisenhardt, Peter, Fruchter, Andrew S., Gonzalez, Anthony H., Goobar, Ariel, Gupta, Ravi R., Hook, Isobel, Jee, M. James, Kim, Alex G., Kowalski, Marek, Lidman, Chris E., Linder, Eric, Luther, Kyle, Nordin, Jakob, Pain, Reynald, Perlmutter, Saul, Raha, Zachary, Rigault, Mickael, Ruiz-Lapuente, Pilar, Saunders, Clare M., Sofiatti, Caroline, Spadafora, Anthony L., Stanford, S. Adam, Stern, Daniel, Suzuki, Nao, and Williams, Steven C.
Abstract: We present the discovery and measurements of a gravitationally lensed supernova (SN) behind the galaxy cluster MOO J1014+0038. Based on multi-band Hubble Space Telescope and Very Large Telescope (VLT) photometry of the supernova, and VLT spectroscopy of the host galaxy, we find a 97.5% probability that this SN is a SN Ia, and a 2.5% chance of a CC SN. Our typing algorithm combines the shape and color of the light curve with the expected rates of each SN type in the host galaxy. With a redshift of 2.2216, this is the highest redshift SN Ia discovered with a spectroscopic host-galaxy redshift. A further distinguishing feature is that the lensing cluster, at redshift 1.23, is the most distant to date to have an amplified SN. The SN lies in the middle of the color and light-curve shape distributions found at lower redshift, disfavoring strong evolution to z = 2.22. We estimate an amplification due to gravitational lensing of 2.8+0.6-0.5 (1.10 +- 0.23 mag)---compatible with the value estimated from the weak-lensing-derived mass and the mass-concentration relation from LambdaCDM simulations---making it the most amplified SN Ia discovered behind a galaxy cluster., Comment: Accepted for publication in ApJ
Published: 2017
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8. The Discovery of a Gravitationally Lensed Supernova Ia at Redshift 2.22

Author: Rubin, David, Hayden, Brian, Huang, Xiaosheng, Aldering, Greg, Amanullah, Rahman, Barbary, Kyle, Boone, Kyle, Brodwin, Mark, Deustua, Susana E., Dixon, Sam, Eisenhardt, Peter, Fruchter, Andrew S., Gonzalez, Anthony H., Goobar, Ariel, Gupta, Ravi R., Hook, Isobel, Jee, M. James, Kim, Alex G., Kowalski, Marek, Lidman, Chris E., Linder, Eric, Luther, Kyle, Nordin, Jakob, Pain, Reynald, Perlmutter, Saul, Raha, Zachary, Rigault, Mickael, Ruiz-Lapuente, Pilar, Saunders, Clare M., Sofiatti, Caroline, Spadafora, Anthony L., Stanford, S. Adam, Stern, Daniel, Suzuki, Nao, Williams, Steven C., Rubin, David, Hayden, Brian, Huang, Xiaosheng, Aldering, Greg, Amanullah, Rahman, Barbary, Kyle, Boone, Kyle, Brodwin, Mark, Deustua, Susana E., Dixon, Sam, Eisenhardt, Peter, Fruchter, Andrew S., Gonzalez, Anthony H., Goobar, Ariel, Gupta, Ravi R., Hook, Isobel, Jee, M. James, Kim, Alex G., Kowalski, Marek, Lidman, Chris E., Linder, Eric, Luther, Kyle, Nordin, Jakob, Pain, Reynald, Perlmutter, Saul, Raha, Zachary, Rigault, Mickael, Ruiz-Lapuente, Pilar, Saunders, Clare M., Sofiatti, Caroline, Spadafora, Anthony L., Stanford, S. Adam, Stern, Daniel, Suzuki, Nao, and Williams, Steven C.
Abstract: We present the discovery and measurements of a gravitationally lensed supernova (SN) behind the galaxy cluster MOO J1014+0038. Based on multi-band Hubble Space Telescope and Very Large Telescope (VLT) photometry of the supernova, and VLT spectroscopy of the host galaxy, we find a 97.5% probability that this SN is a SN Ia, and a 2.5% chance of a CC SN. Our typing algorithm combines the shape and color of the light curve with the expected rates of each SN type in the host galaxy. With a redshift of 2.2216, this is the highest redshift SN Ia discovered with a spectroscopic host-galaxy redshift. A further distinguishing feature is that the lensing cluster, at redshift 1.23, is the most distant to date to have an amplified SN. The SN lies in the middle of the color and light-curve shape distributions found at lower redshift, disfavoring strong evolution to z = 2.22. We estimate an amplification due to gravitational lensing of 2.8+0.6-0.5 (1.10 +- 0.23 mag)---compatible with the value estimated from the weak-lensing-derived mass and the mass-concentration relation from LambdaCDM simulations---making it the most amplified SN Ia discovered behind a galaxy cluster., Comment: Accepted for publication in ApJ
Published: 2017
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9. RAPIDLY RISING TRANSIENTS IN THE SUPERNOVA-SUPERLUMINOUS SUPERNOVA GAP

Author: Arcavi, Iair, Wolf, William M., Howell, D. Andrew, Bildsten, Lars, Leloudas, Giorgos, Hardin, Delphine, Prajs, Szymon, Perley, Daniel A., Svirski, Gilad, Gal-Yam, Avishay, Katz, Boaz, McCully, Curtis, Cenko, S. Bradley, Lidman, Chris, Sullivan, Mark, Valenti, Stefano, Astier, Pierre, Balland, Cristophe, Carlberg, Ray G., Conley, Alex, Fouchez, Dominique, Guy, Julien, Pain, Reynald, Palanque-Delabrouille, Nathalie, Perrett, Kathy, Pritchet, Chris J., Regnault, Nicolas, Rich, James, Ruhlmann-Kleider, Vanina, Arcavi, Iair, Wolf, William M., Howell, D. Andrew, Bildsten, Lars, Leloudas, Giorgos, Hardin, Delphine, Prajs, Szymon, Perley, Daniel A., Svirski, Gilad, Gal-Yam, Avishay, Katz, Boaz, McCully, Curtis, Cenko, S. Bradley, Lidman, Chris, Sullivan, Mark, Valenti, Stefano, Astier, Pierre, Balland, Cristophe, Carlberg, Ray G., Conley, Alex, Fouchez, Dominique, Guy, Julien, Pain, Reynald, Palanque-Delabrouille, Nathalie, Perrett, Kathy, Pritchet, Chris J., Regnault, Nicolas, Rich, James, and Ruhlmann-Kleider, Vanina
Published: 2016

10. Rapidly Rising Transients in the Supernova - Superluminous Supernova Gap

Author: Arcavi, Iair, Wolf, William M., Howell, D. Andrew, Bildsten, Lars, Leloudas, Giorgos, Hardin, Delphine, Prajs, Szymon, Perley, Daniel A., Svirski, Gilad, Gal-Yam, Avishay, Katz, Boaz, McCully, Curtis, Cenko, S. Bradley, Lidman, Chris, Sullivan, Mark, Valenti, Stefano, Astier, Pierre, Balland, Cristophe, Carlberg, Ray G., Conley, Alex, Fouchez, Dominique, Guy, Julien, Pain, Reynald, Palanque-Delabrouille, Nathalie, Perrett, Kathy, Pritchet, Chris J., Regnault, Nicolas, Rich, James, Ruhlmann-Kleider, Vanina, Arcavi, Iair, Wolf, William M., Howell, D. Andrew, Bildsten, Lars, Leloudas, Giorgos, Hardin, Delphine, Prajs, Szymon, Perley, Daniel A., Svirski, Gilad, Gal-Yam, Avishay, Katz, Boaz, McCully, Curtis, Cenko, S. Bradley, Lidman, Chris, Sullivan, Mark, Valenti, Stefano, Astier, Pierre, Balland, Cristophe, Carlberg, Ray G., Conley, Alex, Fouchez, Dominique, Guy, Julien, Pain, Reynald, Palanque-Delabrouille, Nathalie, Perrett, Kathy, Pritchet, Chris J., Regnault, Nicolas, Rich, James, and Ruhlmann-Kleider, Vanina
Abstract: We present observations of four rapidly rising (t_{rise}~10d) transients with peak luminosities between those of supernovae (SNe) and superluminous SNe (M_{peak}~-20) - one discovered and followed by the Palomar Transient Factory (PTF) and three by the Supernova Legacy Survey (SNLS). The light curves resemble those of SN 2011kl, recently shown to be associated with an ultra-long-duration gamma ray burst (GRB), though no GRB was seen to accompany our SNe. The rapid rise to a luminous peak places these events in a unique part of SN phase space, challenging standard SN emission mechanisms. Spectra of the PTF event formally classify it as a Type II SN due to broad Halpha emission, but an unusual absorption feature, which can be interpreted as either high velocity Halpha (though deeper than in previously known cases) or Si II (as seen in Type Ia SNe), is also observed. We find that existing models of white dwarf detonations, CSM interaction, shock breakout in a wind (or steeper CSM) and magnetar spindown can not readily explain the observations. We consider the possibility that a "Type 1.5 SN" scenario could be the origin of our events. More detailed models for these kinds of transients and more constraining observations of future such events should help better determine their nature., Comment: Accepted to ApJ
Published: 2015
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11. Rapidly Rising Transients in the Supernova - Superluminous Supernova Gap

Author: Arcavi, Iair, Wolf, William M., Howell, D. Andrew, Bildsten, Lars, Leloudas, Giorgos, Hardin, Delphine, Prajs, Szymon, Perley, Daniel A., Svirski, Gilad, Gal-Yam, Avishay, Katz, Boaz, McCully, Curtis, Cenko, S. Bradley, Lidman, Chris, Sullivan, Mark, Valenti, Stefano, Astier, Pierre, Balland, Cristophe, Carlberg, Ray G., Conley, Alex, Fouchez, Dominique, Guy, Julien, Pain, Reynald, Palanque-Delabrouille, Nathalie, Perrett, Kathy, Pritchet, Chris J., Regnault, Nicolas, Rich, James, Ruhlmann-Kleider, Vanina, Arcavi, Iair, Wolf, William M., Howell, D. Andrew, Bildsten, Lars, Leloudas, Giorgos, Hardin, Delphine, Prajs, Szymon, Perley, Daniel A., Svirski, Gilad, Gal-Yam, Avishay, Katz, Boaz, McCully, Curtis, Cenko, S. Bradley, Lidman, Chris, Sullivan, Mark, Valenti, Stefano, Astier, Pierre, Balland, Cristophe, Carlberg, Ray G., Conley, Alex, Fouchez, Dominique, Guy, Julien, Pain, Reynald, Palanque-Delabrouille, Nathalie, Perrett, Kathy, Pritchet, Chris J., Regnault, Nicolas, Rich, James, and Ruhlmann-Kleider, Vanina
Abstract: We present observations of four rapidly rising (t_{rise}~10d) transients with peak luminosities between those of supernovae (SNe) and superluminous SNe (M_{peak}~-20) - one discovered and followed by the Palomar Transient Factory (PTF) and three by the Supernova Legacy Survey (SNLS). The light curves resemble those of SN 2011kl, recently shown to be associated with an ultra-long-duration gamma ray burst (GRB), though no GRB was seen to accompany our SNe. The rapid rise to a luminous peak places these events in a unique part of SN phase space, challenging standard SN emission mechanisms. Spectra of the PTF event formally classify it as a Type II SN due to broad Halpha emission, but an unusual absorption feature, which can be interpreted as either high velocity Halpha (though deeper than in previously known cases) or Si II (as seen in Type Ia SNe), is also observed. We find that existing models of white dwarf detonations, CSM interaction, shock breakout in a wind (or steeper CSM) and magnetar spindown can not readily explain the observations. We consider the possibility that a "Type 1.5 SN" scenario could be the origin of our events. More detailed models for these kinds of transients and more constraining observations of future such events should help better determine their nature., Comment: Accepted to ApJ
Published: 2015
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12. The Type Ia supernovae rate with Subaru/XMM-Newton Deep Survey

Author: Okumura, Jun E., Ihara, Yutaka, Doi, Mamoru, Morokuma, Tomoki, Pain, Reynald, Totani, Tomonori, Barbary, Kyle, Takanashi, Naohiro, Yasuda, Naoki, Aldering, Greg, Dawson, Kyle, Goldhaber, Gerson, Hook, Isobel, Lidman, Chris, Perlmutter, Saul, Spadafora, Anthony, Suzuki, Nao, Wang, Lifan, Okumura, Jun E., Ihara, Yutaka, Doi, Mamoru, Morokuma, Tomoki, Pain, Reynald, Totani, Tomonori, Barbary, Kyle, Takanashi, Naohiro, Yasuda, Naoki, Aldering, Greg, Dawson, Kyle, Goldhaber, Gerson, Hook, Isobel, Lidman, Chris, Perlmutter, Saul, Spadafora, Anthony, Suzuki, Nao, and Wang, Lifan
Abstract: We present measurements of the rates of high-redshift Type Ia supernovae derived from the Subaru/XMM-Newton Deep Survey (SXDS). We carried out repeat deep imaging observations with Suprime-Cam on the Subaru Telescope, and detected 1040 variable objects over 0.918 deg$^2$ in the Subaru/XMM-Newton Deep Field. From the imaging observations, light curves in the observed $i'$-band are constructed for all objects, and we fit the observed light curves with template light curves. Out of the 1040 variable objects detected by the SXDS, 39 objects over the redshift range $0.2 < z < 1.4$ are classified as Type Ia supernovae using the light curves. These are among the most distant SN Ia rate measurements to date. We find that the Type Ia supernova rate increase up to $z \sim 0.8$ and may then flatten at higher redshift. The rates can be fitted by a simple power law, $r_V(z)=r_0(1+z)^\alpha$ with $r_0=0.20^{+0.52}_{-0.16}$(stat.)$^{+0.26}_{-0.07}$(syst.)$\times 10^{-4} {\rm yr}^{-1}{\rm Mpc}^{-3}$, and $\alpha=2.04^{+1.84}_{-1.96}$(stat.)$^{+2.11}_{-0.86}$(syst.)., Comment: 21 pages, 16 figures, accepted to PASJ
Published: 2014
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13. The Type Ia supernovae rate with Subaru/XMM-Newton Deep Survey

Author: Okumura, Jun E., Ihara, Yutaka, Doi, Mamoru, Morokuma, Tomoki, Pain, Reynald, Totani, Tomonori, Barbary, Kyle, Takanashi, Naohiro, Yasuda, Naoki, Aldering, Greg, Dawson, Kyle, Goldhaber, Gerson, Hook, Isobel, Lidman, Chris, Perlmutter, Saul, Spadafora, Anthony, Suzuki, Nao, Wang, Lifan, Okumura, Jun E., Ihara, Yutaka, Doi, Mamoru, Morokuma, Tomoki, Pain, Reynald, Totani, Tomonori, Barbary, Kyle, Takanashi, Naohiro, Yasuda, Naoki, Aldering, Greg, Dawson, Kyle, Goldhaber, Gerson, Hook, Isobel, Lidman, Chris, Perlmutter, Saul, Spadafora, Anthony, Suzuki, Nao, and Wang, Lifan
Abstract: We present measurements of the rates of high-redshift Type Ia supernovae derived from the Subaru/XMM-Newton Deep Survey (SXDS). We carried out repeated deep imaging observations with Suprime-Cam on the Subaru Telescope, and detected 1040 variable objects over 0.918 deg(2) in the Subaru/XMM-Newton Deep Field. From the imaging observations, light curves in the observed i band are constructed for all objects, and we fit the observed light curves with template light curves. Out of the 1040 variable objects detected by the SXDS, 39 objects over the redshift range 0.2
Published: 2014

14. The Type Ia supernovae rate with Subaru/XMM-Newton Deep Survey

Author: Okumura, Jun E., Ihara, Yutaka, Doi, Mamoru, Morokuma, Tomoki, Pain, Reynald, Totani, Tomonori, Barbary, Kyle, Takanashi, Naohiro, Yasuda, Naoki, Aldering, Greg, Dawson, Kyle, Goldhaber, Gerson, Hook, Isobel, Lidman, Chris, Perlmutter, Saul, Spadafora, Anthony, Suzuki, Nao, Wang, Lifan, Okumura, Jun E., Ihara, Yutaka, Doi, Mamoru, Morokuma, Tomoki, Pain, Reynald, Totani, Tomonori, Barbary, Kyle, Takanashi, Naohiro, Yasuda, Naoki, Aldering, Greg, Dawson, Kyle, Goldhaber, Gerson, Hook, Isobel, Lidman, Chris, Perlmutter, Saul, Spadafora, Anthony, Suzuki, Nao, and Wang, Lifan
Abstract: We present measurements of the rates of high-redshift Type Ia supernovae derived from the Subaru/XMM-Newton Deep Survey (SXDS). We carried out repeat deep imaging observations with Suprime-Cam on the Subaru Telescope, and detected 1040 variable objects over 0.918 deg$^2$ in the Subaru/XMM-Newton Deep Field. From the imaging observations, light curves in the observed $i'$-band are constructed for all objects, and we fit the observed light curves with template light curves. Out of the 1040 variable objects detected by the SXDS, 39 objects over the redshift range $0.2 < z < 1.4$ are classified as Type Ia supernovae using the light curves. These are among the most distant SN Ia rate measurements to date. We find that the Type Ia supernova rate increase up to $z \sim 0.8$ and may then flatten at higher redshift. The rates can be fitted by a simple power law, $r_V(z)=r_0(1+z)^\alpha$ with $r_0=0.20^{+0.52}_{-0.16}$(stat.)$^{+0.26}_{-0.07}$(syst.)$\times 10^{-4} {\rm yr}^{-1}{\rm Mpc}^{-3}$, and $\alpha=2.04^{+1.84}_{-1.96}$(stat.)$^{+2.11}_{-0.86}$(syst.)., Comment: 21 pages, 16 figures, accepted to PASJ
Published: 2014
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15. Observational Evidence of the Accelerated Expansion of the Universe

Author: Astier, Pierre, Pain, Reynald, Astier, Pierre, and Pain, Reynald
Abstract: The discovery of cosmic acceleration is one of the most important developments in modern cosmology. The observation, thirteen years ago, that type Ia supernovae appear dimmer that they would have been in a decelerating universe followed by a series of independent observations involving galaxies and cluster of galaxies as well as the cosmic microwave background, all point in the same direction: we seem to be living in a flat universe whose expansion is currently undergoing an acceleration phase. In this paper, we review the various observational evidences, most of them gathered in the last decade, and the improvements expected from projects currently collecting data or in preparation., Comment: Accepted review article to appear in a special volume of the "Comptes Rendus de l'Acad\'emie des Sciences" about Dark Energy and Dark Matter
Published: 2012
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16. Observational Evidence of the Accelerated Expansion of the Universe

Author: Astier, Pierre, Pain, Reynald, Astier, Pierre, and Pain, Reynald
Abstract: The discovery of cosmic acceleration is one of the most important developments in modern cosmology. The observation, thirteen years ago, that type Ia supernovae appear dimmer that they would have been in a decelerating universe followed by a series of independent observations involving galaxies and cluster of galaxies as well as the cosmic microwave background, all point in the same direction: we seem to be living in a flat universe whose expansion is currently undergoing an acceleration phase. In this paper, we review the various observational evidences, most of them gathered in the last decade, and the improvements expected from projects currently collecting data or in preparation., Comment: Accepted review article to appear in a special volume of the "Comptes Rendus de l'Acad\'emie des Sciences" about Dark Energy and Dark Matter
Published: 2012
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17. Subaru FOCAS Spectroscopic Observations of High-Redshift Supernovae

Author: Morokuma, Tomoki, Tokita, Kouichi, Lidman, Christopher, Doi, Mamoru, Yasuda, Naoki, Aldering, Greg, Amanullah, Rahman, Barbary, Kyle, Dawson, Kyle, Fadeyev, Vitaliy, Fakhouri, Hannah K., Goldhaber, Gerson, Goobar, Ariel, Hattori, Takashi, Hayano, Junji, Hook, Isobel M., Howell, D. Andrew, Furusawa, Hisanori, Ihara, Yutaka, Kashikawa, Nobunari, Knop, Rob A., Konishi, Kohki, Meyers, Joshua, Oda, Takeshi, Pain, Reynald, Perlmutter, Saul, Rubin, David, Spadafora, Anthony L., Suzuki, Nao, Takanashi, Naohiro, Totani, Tomonori, Utsunomiya, Hiroyuki, Wang, Lifan, Morokuma, Tomoki, Tokita, Kouichi, Lidman, Christopher, Doi, Mamoru, Yasuda, Naoki, Aldering, Greg, Amanullah, Rahman, Barbary, Kyle, Dawson, Kyle, Fadeyev, Vitaliy, Fakhouri, Hannah K., Goldhaber, Gerson, Goobar, Ariel, Hattori, Takashi, Hayano, Junji, Hook, Isobel M., Howell, D. Andrew, Furusawa, Hisanori, Ihara, Yutaka, Kashikawa, Nobunari, Knop, Rob A., Konishi, Kohki, Meyers, Joshua, Oda, Takeshi, Pain, Reynald, Perlmutter, Saul, Rubin, David, Spadafora, Anthony L., Suzuki, Nao, Takanashi, Naohiro, Totani, Tomonori, Utsunomiya, Hiroyuki, and Wang, Lifan
Abstract: We present spectra of high-redshift supernovae (SNe) that were taken with the Subaru low-resolution optical spectrograph, FOCAS. These SNe were found in SN surveys with Suprime-Cam on Subaru, the CFH12k camera on the Canada-France-Hawaii Telescope, and the Advanced Camera for Surveys on the Hubble Space Telescope. These SN surveys specifically targeted z > 1 Type la supernovae (SNe Ia). From the spectra of 39 candidates, we obtained redshifts for 32 candidates and spectroscopically identified 7 active candidates as probable SNe Ia, including one at z = 1.35, which is the most distant SN la to be spectroscopically confirmed with a ground-based telescope. An additional 4 candidates were identified as likely SNe la from the spectrophotometric properties of their host galaxies. Seven candidates are not SNe la, either being SNe of another type or active galactic nuclei. When SNe la were observed within one week of the maximum light, we found that we could spectroscopically identify most of them up to z = 1.1. Beyond this redshift, very few candidates were spectroscopically identified as SNe Ia. The current generation of super red-sensitive, fringe-free CCDs will push this redshift limit higher., authorCount :33
Published: 2010

18. Subaru FOCAS Spectroscopic Observations of High-Redshift Supernovae

Author: Morokuma, Tomoki, Tokita, Kouichi, Lidman, Christopher, Doi, Mamoru, Yasuda, Naoki, Aldering, Greg, Amanullah, Rahman, Barbary, Kyle, Dawson, Kyle, Fadeyev, Vitaliy, Fakhouri, Hannah K., Goldhaber, Gerson, Goobar, Ariel, Hattori, Takashi, Hayano, Junji, Hook, Isobel M., Howell, D. Andrew, Furusawa, Hisanori, Ihara, Yutaka, Kashikawa, Nobunari, Knop, Rob A., Konishi, Kohki, Meyers, Joshua, Oda, Takeshi, Pain, Reynald, Perlmutter, Saul, Rubin, David, Spadafora, Anthony L., Suzuki, Nao, Takanashi, Naohiro, Totani, Tomonori, Utsunomiya, Hiroyuki, Wang, Lifan, Morokuma, Tomoki, Tokita, Kouichi, Lidman, Christopher, Doi, Mamoru, Yasuda, Naoki, Aldering, Greg, Amanullah, Rahman, Barbary, Kyle, Dawson, Kyle, Fadeyev, Vitaliy, Fakhouri, Hannah K., Goldhaber, Gerson, Goobar, Ariel, Hattori, Takashi, Hayano, Junji, Hook, Isobel M., Howell, D. Andrew, Furusawa, Hisanori, Ihara, Yutaka, Kashikawa, Nobunari, Knop, Rob A., Konishi, Kohki, Meyers, Joshua, Oda, Takeshi, Pain, Reynald, Perlmutter, Saul, Rubin, David, Spadafora, Anthony L., Suzuki, Nao, Takanashi, Naohiro, Totani, Tomonori, Utsunomiya, Hiroyuki, and Wang, Lifan
Abstract: We present spectra of high-redshift supernovae (SNe) that were taken with the Subaru low resolution optical spectrograph, FOCAS. These SNe were found in SN surveys with Suprime-Cam on Subaru, the CFH12k camera on the Canada-France-Hawaii Telescope (CFHT), and the Advanced Camera for Surveys (ACS) on the Hubble Space Telescope (HST). These SN surveys specifically targeted z>1 Type Ia supernovae (SNe Ia). From the spectra of 39 candidates, we obtain redshifts for 32 candidates and spectroscopically identify 7 active candidates as probable SNe Ia, including one at z=1.35, which is the most distant SN Ia to be spectroscopically confirmed with a ground-based telescope. An additional 4 candidates are identified as likely SNe Ia from the spectrophotometric properties of their host galaxies. Seven candidates are not SNe Ia, either being SNe of another type or active galactic nuclei. When SNe Ia are observed within a week of maximum light, we find that we can spectroscopically identify most of them up to z=1.1. Beyond this redshift, very few candidates were spectroscopically identified as SNe Ia. The current generation of super red-sensitive, fringe-free CCDs will push this redshift limit higher., Comment: 19 pages, 26 figures. PASJ in press. see http://www.supernova.lbl.gov/2009ClusterSurvey/ for additional information pertaining to the HST Cluster SN Survey
Published: 2009
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19. Subaru FOCAS Spectroscopic Observations of High-Redshift Supernovae

Author: Morokuma, Tomoki, Tokita, Kouichi, Lidman, Christopher, Doi, Mamoru, Yasuda, Naoki, Aldering, Greg, Amanullah, Rahman, Barbary, Kyle, Dawson, Kyle, Fadeyev, Vitaliy, Fakhouri, Hannah K., Goldhaber, Gerson, Goobar, Ariel, Hattori, Takashi, Hayano, Junji, Hook, Isobel M., Howell, D. Andrew, Furusawa, Hisanori, Ihara, Yutaka, Kashikawa, Nobunari, Knop, Rob A., Konishi, Kohki, Meyers, Joshua, Oda, Takeshi, Pain, Reynald, Perlmutter, Saul, Rubin, David, Spadafora, Anthony L., Suzuki, Nao, Takanashi, Naohiro, Totani, Tomonori, Utsunomiya, Hiroyuki, Wang, Lifan, Morokuma, Tomoki, Tokita, Kouichi, Lidman, Christopher, Doi, Mamoru, Yasuda, Naoki, Aldering, Greg, Amanullah, Rahman, Barbary, Kyle, Dawson, Kyle, Fadeyev, Vitaliy, Fakhouri, Hannah K., Goldhaber, Gerson, Goobar, Ariel, Hattori, Takashi, Hayano, Junji, Hook, Isobel M., Howell, D. Andrew, Furusawa, Hisanori, Ihara, Yutaka, Kashikawa, Nobunari, Knop, Rob A., Konishi, Kohki, Meyers, Joshua, Oda, Takeshi, Pain, Reynald, Perlmutter, Saul, Rubin, David, Spadafora, Anthony L., Suzuki, Nao, Takanashi, Naohiro, Totani, Tomonori, Utsunomiya, Hiroyuki, and Wang, Lifan
Abstract: We present spectra of high-redshift supernovae (SNe) that were taken with the Subaru low resolution optical spectrograph, FOCAS. These SNe were found in SN surveys with Suprime-Cam on Subaru, the CFH12k camera on the Canada-France-Hawaii Telescope (CFHT), and the Advanced Camera for Surveys (ACS) on the Hubble Space Telescope (HST). These SN surveys specifically targeted z>1 Type Ia supernovae (SNe Ia). From the spectra of 39 candidates, we obtain redshifts for 32 candidates and spectroscopically identify 7 active candidates as probable SNe Ia, including one at z=1.35, which is the most distant SN Ia to be spectroscopically confirmed with a ground-based telescope. An additional 4 candidates are identified as likely SNe Ia from the spectrophotometric properties of their host galaxies. Seven candidates are not SNe Ia, either being SNe of another type or active galactic nuclei. When SNe Ia are observed within a week of maximum light, we find that we can spectroscopically identify most of them up to z=1.1. Beyond this redshift, very few candidates were spectroscopically identified as SNe Ia. The current generation of super red-sensitive, fringe-free CCDs will push this redshift limit higher., Comment: 19 pages, 26 figures. PASJ in press. see http://www.supernova.lbl.gov/2009ClusterSurvey/ for additional information pertaining to the HST Cluster SN Survey
Published: 2009
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20. The type Ia supernova SNLS-03D3bb from a super-Chandrasekhar-mass white dwarf star

Author: Howell, D.Andrew, Howell, D.Andrew, Sullivan, Mark, Nugent, Peter E., Ellis, Richard S., Conley, Alexander J., Le Borgne, Damien, Carlberg, Raymond G., Guy, Julien, Balam, David, Basa, Stephane, Fouchez, Dominique, Hook, Isobel M., Hsiao, Eric Y., Neill, James D., Pain, Reynald, Perrett, Kathryn M., Pritchet, Christopher J., Howell, D.Andrew, Howell, D.Andrew, Sullivan, Mark, Nugent, Peter E., Ellis, Richard S., Conley, Alexander J., Le Borgne, Damien, Carlberg, Raymond G., Guy, Julien, Balam, David, Basa, Stephane, Fouchez, Dominique, Hook, Isobel M., Hsiao, Eric Y., Neill, James D., Pain, Reynald, Perrett, Kathryn M., and Pritchet, Christopher J.
Abstract: The acceleration of the expansion of the universe, and the need for Dark Energy, were inferred from the observations of Type Ia supernovae (SNe Ia) 1;2. There is consensus that SNeIa are thermonuclear explosions that destroy carbon-oxygen white dwarf stars that accrete matter from a companion star3, although the nature of this companion remains uncertain. SNe Ia are thought to be reliable distance indicators because they have a standard amount of fuel and a uniform trigger they are predicted to explode when the mass of the white dwarf nears the Chandrasekhar mass 4 - 1.4 solar masses. Here we show that the high redshift supernova SNLS-03D3bb has an exceptionally high luminosity and low kinetic energy that both imply a super-Chandrasekhar mass progenitor. Super-Chandrasekhar mass SNeIa should preferentially occur in a young stellar population, so this may provide an explanation for the observed trend that overluminous SNe Ia only occur in young environments5;6. Since this supernova does not obey the relations that allow them to be calibrated as standard candles, and since no counterparts have been found at low redshift, future cosmology studies will have to consider contamination from such events.
Published: 2008

21. LSST: from Science Drivers to Reference Design and Anticipated Data Products

Author: Ivezić, Željko, Kahn, Steven M., Tyson, J. Anthony, Abel, Bob, Acosta, Emily, Allsman, Robyn, Alonso, David, AlSayyad, Yusra, Anderson, Scott F., Andrew, John, Angel, James Roger P., Angeli, George Z., Ansari, Reza, Antilogus, Pierre, Araujo, Constanza, Armstrong, Robert, Arndt, Kirk T., Astier, Pierre, Aubourg, Éric, Auza, Nicole, Axelrod, Tim S., Bard, Deborah J., Barr, Jeff D., Barrau, Aurelian, Bartlett, James G., Bauer, Amanda E., Bauman, Brian J., Baumont, Sylvain, Becker, Andrew C., Becla, Jacek, Beldica, Cristina, Bellavia, Steve, Bianco, Federica B., Biswas, Rahul, Blanc, Guillaume, Blazek, Jonathan, Blandford, Roger D., Bloom, Josh S., Bogart, Joanne, Bond, Tim W., Borgland, Anders W., Borne, Kirk, Bosch, James F., Boutigny, Dominique, Brackett, Craig A., Bradshaw, Andrew, Brandt, William Nielsen, Brown, Michael E., Bullock, James S., Burchat, Patricia, Burke, David L., Cagnoli, Gianpietro, Calabrese, Daniel, Callahan, Shawn, Callen, Alice L., Chandrasekharan, Srinivasan, Charles-Emerson, Glenaver, Chesley, Steve, Cheu, Elliott C., Chiang, Hsin-Fang, Chiang, James, Chirino, Carol, Chow, Derek, Ciardi, David R., Claver, Charles F., Cohen-Tanugi, Johann, Cockrum, Joseph J., Coles, Rebecca, Connolly, Andrew J., Cook, Kem H., Cooray, Asantha, Covey, Kevin R., Cribbs, Chris, Cui, Wei, Cutri, Roc, Daly, Philip N., Daniel, Scott F., Daruich, Felipe, Daubard, Guillaume, Daues, Greg, Dawson, William, Delgado, Francisco, Dellapenna, Alfred, de Peyster, Robert, de Val-Borro, Miguel, Digel, Seth W., Doherty, Peter, Dubois, Richard, Dubois-Felsmann, Gregory P., Durech, Josef, Economou, Frossie, Eracleous, Michael, Ferguson, Henry, Figueroa, Enrique, Fisher-Levine, Merlin, Focke, Warren, Foss, Michael D., Frank, James, Freemon, Michael D., Gangler, Emmanuel, Gawiser, Eric, Geary, John C., Gee, Perry, Geha, Marla, Gessner, Charles J. B., Gibson, Robert R., Gilmore, D. Kirk, Glanzman, Thomas, Glick, William, Goldina, Tatiana, Goldstein, Daniel A., Goodenow, Iain, Graham, Melissa L., Gressler, William J., Gris, Philippe, Guy, Leanne P., Guyonnet, Augustin, Haller, Gunther, Harris, Ron, Hascall, Patrick A., Haupt, Justine, Hernandez, Fabio, Herrmann, Sven, Hileman, Edward, Hoblitt, Joshua, Hodgson, John A., Hogan, Craig, Huang, Dajun, Huffer, Michael E., Ingraham, Patrick, Innes, Walter R., Jacoby, Suzanne H., Jain, Bhuvnesh, Jammes, Fabrice, Jee, James, Jenness, Tim, Jernigan, Garrett, Jevremović, Darko, Johns, Kenneth, Johnson, Anthony S., Johnson, Margaret W. G., Jones, R. Lynne, Juramy-Gilles, Claire, Jurić, Mario, Kalirai, Jason S., Kallivayalil, Nitya J., Kalmbach, Bryce, Kantor, Jeffrey P., Karst, Pierre, Kasliwal, Mansi M., Kelly, Heather, Kessler, Richard, Kinnison, Veronica, Kirkby, David, Knox, Lloyd, Kotov, Ivan V., Krabbendam, Victor L., Krughoff, K. Simon, Kubánek, Petr, Kuczewski, John, Kulkarni, Shri, Ku, John, Kurita, Nadine R., Lage, Craig S., Lambert, Ron, Lange, Travis, Langton, J. Brian, Guillou, Laurent Le, Levine, Deborah, Liang, Ming, Lim, Kian-Tat, Lintott, Chris J., Long, Kevin E., Lopez, Margaux, Lotz, Paul J., Lupton, Robert H., Lust, Nate B., MacArthur, Lauren A., Mahabal, Ashish, Mandelbaum, Rachel, Marsh, Darren S., Marshall, Philip J., Marshall, Stuart, May, Morgan, McKercher, Robert, McQueen, Michelle, Meyers, Joshua, Migliore, Myriam, Miller, Michelle, Mills, David J., Miraval, Connor, Moeyens, Joachim, Monet, David G., Moniez, Marc, Monkewitz, Serge, Montgomery, Christopher, Mueller, Fritz, Muller, Gary P., Arancibia, Freddy Muñoz, Neill, Douglas R., Newbry, Scott P., Nief, Jean-Yves, Nomerotski, Andrei, Nordby, Martin, O'Connor, Paul, Oliver, John, Olivier, Scot S., Olsen, Knut, O'Mullane, William, Ortiz, Sandra, Osier, Shawn, Owen, Russell E., Pain, Reynald, Palecek, Paul E., Parejko, John K., Parsons, James B., Pease, Nathan M., Peterson, J. Matt, Peterson, John R., Petravick, Donald L., Petrick, M. E. Libby, Petry, Cathy E., Pierfederici, Francesco, Pietrowicz, Stephen, Pike, Rob, Pinto, Philip A., Plante, Raymond, Plate, Stephen, Price, Paul A., Prouza, Michael, Radeka, Veljko, Rajagopal, Jayadev, Rasmussen, Andrew P., Regnault, Nicolas, Reil, Kevin A., Reiss, David J., Reuter, Michael A., Ridgway, Stephen T., Riot, Vincent J., Ritz, Steve, Robinson, Sean, Roby, William, Roodman, Aaron, Rosing, Wayne, Roucelle, Cecille, Rumore, Matthew R., Russo, Stefano, Saha, Abhijit, Sassolas, Benoit, Schalk, Terry L., Schellart, Pim, Schindler, Rafe H., Schmidt, Samuel, Schneider, Donald P., Schneider, Michael D., Schoening, William, Schumacher, German, Schwamb, Megan E., Sebag, Jacques, Selvy, Brian, Sembroski, Glenn H., Seppala, Lynn G., Serio, Andrew, Serrano, Eduardo, Shaw, Richard A., Shipsey, Ian, Sick, Jonathan, Silvestri, Nicole, Slater, Colin T., Smith, J. Allyn, Smith, R. Chris, Sobhani, Shahram, Soldahl, Christine, Storrie-Lombardi, Lisa, Stover, Edward, Strauss, Michael A., Street, Rachel A., Stubbs, Christopher W., Sullivan, Ian S., Sweeney, Donald, Swinbank, John D., Szalay, Alexander, Takacs, Peter, Tether, Stephen A., Thaler, Jon J., Thayer, John Gregg, Thomas, Sandrine, Thukral, Vaikunth, Tice, Jeffrey, Trilling, David E., Turri, Max, Van Berg, Richard, Berk, Daniel Vanden, Vetter, Kurt, Virieux, Francoise, Vucina, Tomislav, Wahl, William, Walkowicz, Lucianne, Walsh, Brian, Walter, Christopher W., Wang, Daniel L., Wang, Shin-Yawn, Warner, Michael, Wiecha, Oliver, Willman, Beth, Winters, Scott E., Wittman, David, Wolff, Sidney C., Wood-Vasey, W. Michael, Wu, Xiuqin, Xin, Bo, Yoachim, Peter, Zhan, Hu, Ivezić, Željko, Kahn, Steven M., Tyson, J. Anthony, Abel, Bob, Acosta, Emily, Allsman, Robyn, Alonso, David, AlSayyad, Yusra, Anderson, Scott F., Andrew, John, Angel, James Roger P., Angeli, George Z., Ansari, Reza, Antilogus, Pierre, Araujo, Constanza, Armstrong, Robert, Arndt, Kirk T., Astier, Pierre, Aubourg, Éric, Auza, Nicole, Axelrod, Tim S., Bard, Deborah J., Barr, Jeff D., Barrau, Aurelian, Bartlett, James G., Bauer, Amanda E., Bauman, Brian J., Baumont, Sylvain, Becker, Andrew C., Becla, Jacek, Beldica, Cristina, Bellavia, Steve, Bianco, Federica B., Biswas, Rahul, Blanc, Guillaume, Blazek, Jonathan, Blandford, Roger D., Bloom, Josh S., Bogart, Joanne, Bond, Tim W., Borgland, Anders W., Borne, Kirk, Bosch, James F., Boutigny, Dominique, Brackett, Craig A., Bradshaw, Andrew, Brandt, William Nielsen, Brown, Michael E., Bullock, James S., Burchat, Patricia, Burke, David L., Cagnoli, Gianpietro, Calabrese, Daniel, Callahan, Shawn, Callen, Alice L., Chandrasekharan, Srinivasan, Charles-Emerson, Glenaver, Chesley, Steve, Cheu, Elliott C., Chiang, Hsin-Fang, Chiang, James, Chirino, Carol, Chow, Derek, Ciardi, David R., Claver, Charles F., Cohen-Tanugi, Johann, Cockrum, Joseph J., Coles, Rebecca, Connolly, Andrew J., Cook, Kem H., Cooray, Asantha, Covey, Kevin R., Cribbs, Chris, Cui, Wei, Cutri, Roc, Daly, Philip N., Daniel, Scott F., Daruich, Felipe, Daubard, Guillaume, Daues, Greg, Dawson, William, Delgado, Francisco, Dellapenna, Alfred, de Peyster, Robert, de Val-Borro, Miguel, Digel, Seth W., Doherty, Peter, Dubois, Richard, Dubois-Felsmann, Gregory P., Durech, Josef, Economou, Frossie, Eracleous, Michael, Ferguson, Henry, Figueroa, Enrique, Fisher-Levine, Merlin, Focke, Warren, Foss, Michael D., Frank, James, Freemon, Michael D., Gangler, Emmanuel, Gawiser, Eric, Geary, John C., Gee, Perry, Geha, Marla, Gessner, Charles J. B., Gibson, Robert R., Gilmore, D. Kirk, Glanzman, Thomas, Glick, William, Goldina, Tatiana, Goldstein, Daniel A., Goodenow, Iain, Graham, Melissa L., Gressler, William J., Gris, Philippe, Guy, Leanne P., Guyonnet, Augustin, Haller, Gunther, Harris, Ron, Hascall, Patrick A., Haupt, Justine, Hernandez, Fabio, Herrmann, Sven, Hileman, Edward, Hoblitt, Joshua, Hodgson, John A., Hogan, Craig, Huang, Dajun, Huffer, Michael E., Ingraham, Patrick, Innes, Walter R., Jacoby, Suzanne H., Jain, Bhuvnesh, Jammes, Fabrice, Jee, James, Jenness, Tim, Jernigan, Garrett, Jevremović, Darko, Johns, Kenneth, Johnson, Anthony S., Johnson, Margaret W. G., Jones, R. Lynne, Juramy-Gilles, Claire, Jurić, Mario, Kalirai, Jason S., Kallivayalil, Nitya J., Kalmbach, Bryce, Kantor, Jeffrey P., Karst, Pierre, Kasliwal, Mansi M., Kelly, Heather, Kessler, Richard, Kinnison, Veronica, Kirkby, David, Knox, Lloyd, Kotov, Ivan V., Krabbendam, Victor L., Krughoff, K. Simon, Kubánek, Petr, Kuczewski, John, Kulkarni, Shri, Ku, John, Kurita, Nadine R., Lage, Craig S., Lambert, Ron, Lange, Travis, Langton, J. Brian, Guillou, Laurent Le, Levine, Deborah, Liang, Ming, Lim, Kian-Tat, Lintott, Chris J., Long, Kevin E., Lopez, Margaux, Lotz, Paul J., Lupton, Robert H., Lust, Nate B., MacArthur, Lauren A., Mahabal, Ashish, Mandelbaum, Rachel, Marsh, Darren S., Marshall, Philip J., Marshall, Stuart, May, Morgan, McKercher, Robert, McQueen, Michelle, Meyers, Joshua, Migliore, Myriam, Miller, Michelle, Mills, David J., Miraval, Connor, Moeyens, Joachim, Monet, David G., Moniez, Marc, Monkewitz, Serge, Montgomery, Christopher, Mueller, Fritz, Muller, Gary P., Arancibia, Freddy Muñoz, Neill, Douglas R., Newbry, Scott P., Nief, Jean-Yves, Nomerotski, Andrei, Nordby, Martin, O'Connor, Paul, Oliver, John, Olivier, Scot S., Olsen, Knut, O'Mullane, William, Ortiz, Sandra, Osier, Shawn, Owen, Russell E., Pain, Reynald, Palecek, Paul E., Parejko, John K., Parsons, James B., Pease, Nathan M., Peterson, J. Matt, Peterson, John R., Petravick, Donald L., Petrick, M. E. Libby, Petry, Cathy E., Pierfederici, Francesco, Pietrowicz, Stephen, Pike, Rob, Pinto, Philip A., Plante, Raymond, Plate, Stephen, Price, Paul A., Prouza, Michael, Radeka, Veljko, Rajagopal, Jayadev, Rasmussen, Andrew P., Regnault, Nicolas, Reil, Kevin A., Reiss, David J., Reuter, Michael A., Ridgway, Stephen T., Riot, Vincent J., Ritz, Steve, Robinson, Sean, Roby, William, Roodman, Aaron, Rosing, Wayne, Roucelle, Cecille, Rumore, Matthew R., Russo, Stefano, Saha, Abhijit, Sassolas, Benoit, Schalk, Terry L., Schellart, Pim, Schindler, Rafe H., Schmidt, Samuel, Schneider, Donald P., Schneider, Michael D., Schoening, William, Schumacher, German, Schwamb, Megan E., Sebag, Jacques, Selvy, Brian, Sembroski, Glenn H., Seppala, Lynn G., Serio, Andrew, Serrano, Eduardo, Shaw, Richard A., Shipsey, Ian, Sick, Jonathan, Silvestri, Nicole, Slater, Colin T., Smith, J. Allyn, Smith, R. Chris, Sobhani, Shahram, Soldahl, Christine, Storrie-Lombardi, Lisa, Stover, Edward, Strauss, Michael A., Street, Rachel A., Stubbs, Christopher W., Sullivan, Ian S., Sweeney, Donald, Swinbank, John D., Szalay, Alexander, Takacs, Peter, Tether, Stephen A., Thaler, Jon J., Thayer, John Gregg, Thomas, Sandrine, Thukral, Vaikunth, Tice, Jeffrey, Trilling, David E., Turri, Max, Van Berg, Richard, Berk, Daniel Vanden, Vetter, Kurt, Virieux, Francoise, Vucina, Tomislav, Wahl, William, Walkowicz, Lucianne, Walsh, Brian, Walter, Christopher W., Wang, Daniel L., Wang, Shin-Yawn, Warner, Michael, Wiecha, Oliver, Willman, Beth, Winters, Scott E., Wittman, David, Wolff, Sidney C., Wood-Vasey, W. Michael, Wu, Xiuqin, Xin, Bo, Yoachim, Peter, and Zhan, Hu
Abstract: (Abridged) We describe here the most ambitious survey currently planned in the optical, the Large Synoptic Survey Telescope (LSST). A vast array of science will be enabled by a single wide-deep-fast sky survey, and LSST will have unique survey capability in the faint time domain. The LSST design is driven by four main science themes: probing dark energy and dark matter, taking an inventory of the Solar System, exploring the transient optical sky, and mapping the Milky Way. LSST will be a wide-field ground-based system sited at Cerro Pach\'{o}n in northern Chile. The telescope will have an 8.4 m (6.5 m effective) primary mirror, a 9.6 deg$^2$ field of view, and a 3.2 Gigapixel camera. The standard observing sequence will consist of pairs of 15-second exposures in a given field, with two such visits in each pointing in a given night. With these repeats, the LSST system is capable of imaging about 10,000 square degrees of sky in a single filter in three nights. The typical 5$\sigma$ point-source depth in a single visit in $r$ will be $\sim 24.5$ (AB). The project is in the construction phase and will begin regular survey operations by 2022. The survey area will be contained within 30,000 deg$^2$ with $\delta<+34.5^\circ$, and will be imaged multiple times in six bands, $ugrizy$, covering the wavelength range 320--1050 nm. About 90\% of the observing time will be devoted to a deep-wide-fast survey mode which will uniformly observe a 18,000 deg$^2$ region about 800 times (summed over all six bands) during the anticipated 10 years of operations, and yield a coadded map to $r\sim27.5$. The remaining 10\% of the observing time will be allocated to projects such as a Very Deep and Fast time domain survey. The goal is to make LSST data products, including a relational database of about 32 trillion observations of 40 billion objects, available to the public and scientists around the world., Comment: 57 pages, 32 color figures, version with high-resolution figures available from https://www.lsst.org/overview
Published: 2008
Full Text: View/download PDF

22. Supernova Shock Breakout from a Red Supergiant

Author: Schawinski, Kevin, Justham, Stephen, Wolf, Christian, Podsiadlowski, Philipp, Sullivan, Mark, Steenbrugge, Katrien C., Bell, Tony, Roeser, Hermann-Josef, Walker, Emma, Astier, Pierre, Balam, Dave, Balland, Christophe, Carlberg, Ray, Conley, Alex, Fouchez, Dominque, Guy, Julien, Hardin, Delphine, Hook, Isobel, Howell, Andy, Pain, Reynald, Perrett, Kathy, Pritchet, Chris, Regnault, Nicolas, Yi, Sukyoung K., Schawinski, Kevin, Justham, Stephen, Wolf, Christian, Podsiadlowski, Philipp, Sullivan, Mark, Steenbrugge, Katrien C., Bell, Tony, Roeser, Hermann-Josef, Walker, Emma, Astier, Pierre, Balam, Dave, Balland, Christophe, Carlberg, Ray, Conley, Alex, Fouchez, Dominque, Guy, Julien, Hardin, Delphine, Hook, Isobel, Howell, Andy, Pain, Reynald, Perrett, Kathy, Pritchet, Chris, Regnault, Nicolas, and Yi, Sukyoung K.
Abstract: Massive stars undergo a violent death when the supply of nuclear fuel in their cores is exhausted, resulting in a catastrophic "core-collapse" supernova. Such events are usually only detected at least a few days after the star has exploded. Observations of the supernova SNLS-04D2dc with the Galaxy Evolution Explorer space telescope reveal a radiative precursor from the supernova shock before the shock reached the surface of the star and show the initial expansion of the star at the beginning of the explosion. Theoretical models of the ultraviolet light curve confirm that the progenitor was a red supergiant, as expected for this type of supernova. These observations provide a way to probe the physics of core-collapse supernovae and the internal structures of their progenitor stars, Comment: Science, in press. 32 pages, 7 figures
Published: 2008
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23. The type Ia supernova SNLS-03D3bb from a super-Chandrasekhar-mass white dwarf star

Author: Howell, D.Andrew, Howell, D.Andrew, Sullivan, Mark, Nugent, Peter E., Ellis, Richard S., Conley, Alexander J., Le Borgne, Damien, Carlberg, Raymond G., Guy, Julien, Balam, David, Basa, Stephane, Fouchez, Dominique, Hook, Isobel M., Hsiao, Eric Y., Neill, James D., Pain, Reynald, Perrett, Kathryn M., Pritchet, Christopher J., Howell, D.Andrew, Howell, D.Andrew, Sullivan, Mark, Nugent, Peter E., Ellis, Richard S., Conley, Alexander J., Le Borgne, Damien, Carlberg, Raymond G., Guy, Julien, Balam, David, Basa, Stephane, Fouchez, Dominique, Hook, Isobel M., Hsiao, Eric Y., Neill, James D., Pain, Reynald, Perrett, Kathryn M., and Pritchet, Christopher J.
Abstract: The acceleration of the expansion of the universe, and the need for Dark Energy, were inferred from the observations of Type Ia supernovae (SNe Ia) 1;2. There is consensus that SNeIa are thermonuclear explosions that destroy carbon-oxygen white dwarf stars that accrete matter from a companion star3, although the nature of this companion remains uncertain. SNe Ia are thought to be reliable distance indicators because they have a standard amount of fuel and a uniform trigger they are predicted to explode when the mass of the white dwarf nears the Chandrasekhar mass 4 - 1.4 solar masses. Here we show that the high redshift supernova SNLS-03D3bb has an exceptionally high luminosity and low kinetic energy that both imply a super-Chandrasekhar mass progenitor. Super-Chandrasekhar mass SNeIa should preferentially occur in a young stellar population, so this may provide an explanation for the observed trend that overluminous SNe Ia only occur in young environments5;6. Since this supernova does not obey the relations that allow them to be calibrated as standard candles, and since no counterparts have been found at low redshift, future cosmology studies will have to consider contamination from such events.
Published: 2008

24. LSST: from Science Drivers to Reference Design and Anticipated Data Products

Author: Ivezić, Željko, Kahn, Steven M., Tyson, J. Anthony, Abel, Bob, Acosta, Emily, Allsman, Robyn, Alonso, David, AlSayyad, Yusra, Anderson, Scott F., Andrew, John, Angel, James Roger P., Angeli, George Z., Ansari, Reza, Antilogus, Pierre, Araujo, Constanza, Armstrong, Robert, Arndt, Kirk T., Astier, Pierre, Aubourg, Éric, Auza, Nicole, Axelrod, Tim S., Bard, Deborah J., Barr, Jeff D., Barrau, Aurelian, Bartlett, James G., Bauer, Amanda E., Bauman, Brian J., Baumont, Sylvain, Becker, Andrew C., Becla, Jacek, Beldica, Cristina, Bellavia, Steve, Bianco, Federica B., Biswas, Rahul, Blanc, Guillaume, Blazek, Jonathan, Blandford, Roger D., Bloom, Josh S., Bogart, Joanne, Bond, Tim W., Borgland, Anders W., Borne, Kirk, Bosch, James F., Boutigny, Dominique, Brackett, Craig A., Bradshaw, Andrew, Brandt, William Nielsen, Brown, Michael E., Bullock, James S., Burchat, Patricia, Burke, David L., Cagnoli, Gianpietro, Calabrese, Daniel, Callahan, Shawn, Callen, Alice L., Chandrasekharan, Srinivasan, Charles-Emerson, Glenaver, Chesley, Steve, Cheu, Elliott C., Chiang, Hsin-Fang, Chiang, James, Chirino, Carol, Chow, Derek, Ciardi, David R., Claver, Charles F., Cohen-Tanugi, Johann, Cockrum, Joseph J., Coles, Rebecca, Connolly, Andrew J., Cook, Kem H., Cooray, Asantha, Covey, Kevin R., Cribbs, Chris, Cui, Wei, Cutri, Roc, Daly, Philip N., Daniel, Scott F., Daruich, Felipe, Daubard, Guillaume, Daues, Greg, Dawson, William, Delgado, Francisco, Dellapenna, Alfred, de Peyster, Robert, de Val-Borro, Miguel, Digel, Seth W., Doherty, Peter, Dubois, Richard, Dubois-Felsmann, Gregory P., Durech, Josef, Economou, Frossie, Eracleous, Michael, Ferguson, Henry, Figueroa, Enrique, Fisher-Levine, Merlin, Focke, Warren, Foss, Michael D., Frank, James, Freemon, Michael D., Gangler, Emmanuel, Gawiser, Eric, Geary, John C., Gee, Perry, Geha, Marla, Gessner, Charles J. B., Gibson, Robert R., Gilmore, D. Kirk, Glanzman, Thomas, Glick, William, Goldina, Tatiana, Goldstein, Daniel A., Goodenow, Iain, Graham, Melissa L., Gressler, William J., Gris, Philippe, Guy, Leanne P., Guyonnet, Augustin, Haller, Gunther, Harris, Ron, Hascall, Patrick A., Haupt, Justine, Hernandez, Fabio, Herrmann, Sven, Hileman, Edward, Hoblitt, Joshua, Hodgson, John A., Hogan, Craig, Huang, Dajun, Huffer, Michael E., Ingraham, Patrick, Innes, Walter R., Jacoby, Suzanne H., Jain, Bhuvnesh, Jammes, Fabrice, Jee, James, Jenness, Tim, Jernigan, Garrett, Jevremović, Darko, Johns, Kenneth, Johnson, Anthony S., Johnson, Margaret W. G., Jones, R. Lynne, Juramy-Gilles, Claire, Jurić, Mario, Kalirai, Jason S., Kallivayalil, Nitya J., Kalmbach, Bryce, Kantor, Jeffrey P., Karst, Pierre, Kasliwal, Mansi M., Kelly, Heather, Kessler, Richard, Kinnison, Veronica, Kirkby, David, Knox, Lloyd, Kotov, Ivan V., Krabbendam, Victor L., Krughoff, K. Simon, Kubánek, Petr, Kuczewski, John, Kulkarni, Shri, Ku, John, Kurita, Nadine R., Lage, Craig S., Lambert, Ron, Lange, Travis, Langton, J. Brian, Guillou, Laurent Le, Levine, Deborah, Liang, Ming, Lim, Kian-Tat, Lintott, Chris J., Long, Kevin E., Lopez, Margaux, Lotz, Paul J., Lupton, Robert H., Lust, Nate B., MacArthur, Lauren A., Mahabal, Ashish, Mandelbaum, Rachel, Marsh, Darren S., Marshall, Philip J., Marshall, Stuart, May, Morgan, McKercher, Robert, McQueen, Michelle, Meyers, Joshua, Migliore, Myriam, Miller, Michelle, Mills, David J., Miraval, Connor, Moeyens, Joachim, Monet, David G., Moniez, Marc, Monkewitz, Serge, Montgomery, Christopher, Mueller, Fritz, Muller, Gary P., Arancibia, Freddy Muñoz, Neill, Douglas R., Newbry, Scott P., Nief, Jean-Yves, Nomerotski, Andrei, Nordby, Martin, O'Connor, Paul, Oliver, John, Olivier, Scot S., Olsen, Knut, O'Mullane, William, Ortiz, Sandra, Osier, Shawn, Owen, Russell E., Pain, Reynald, Palecek, Paul E., Parejko, John K., Parsons, James B., Pease, Nathan M., Peterson, J. Matt, Peterson, John R., Petravick, Donald L., Petrick, M. E. Libby, Petry, Cathy E., Pierfederici, Francesco, Pietrowicz, Stephen, Pike, Rob, Pinto, Philip A., Plante, Raymond, Plate, Stephen, Price, Paul A., Prouza, Michael, Radeka, Veljko, Rajagopal, Jayadev, Rasmussen, Andrew P., Regnault, Nicolas, Reil, Kevin A., Reiss, David J., Reuter, Michael A., Ridgway, Stephen T., Riot, Vincent J., Ritz, Steve, Robinson, Sean, Roby, William, Roodman, Aaron, Rosing, Wayne, Roucelle, Cecille, Rumore, Matthew R., Russo, Stefano, Saha, Abhijit, Sassolas, Benoit, Schalk, Terry L., Schellart, Pim, Schindler, Rafe H., Schmidt, Samuel, Schneider, Donald P., Schneider, Michael D., Schoening, William, Schumacher, German, Schwamb, Megan E., Sebag, Jacques, Selvy, Brian, Sembroski, Glenn H., Seppala, Lynn G., Serio, Andrew, Serrano, Eduardo, Shaw, Richard A., Shipsey, Ian, Sick, Jonathan, Silvestri, Nicole, Slater, Colin T., Smith, J. Allyn, Smith, R. Chris, Sobhani, Shahram, Soldahl, Christine, Storrie-Lombardi, Lisa, Stover, Edward, Strauss, Michael A., Street, Rachel A., Stubbs, Christopher W., Sullivan, Ian S., Sweeney, Donald, Swinbank, John D., Szalay, Alexander, Takacs, Peter, Tether, Stephen A., Thaler, Jon J., Thayer, John Gregg, Thomas, Sandrine, Thukral, Vaikunth, Tice, Jeffrey, Trilling, David E., Turri, Max, Van Berg, Richard, Berk, Daniel Vanden, Vetter, Kurt, Virieux, Francoise, Vucina, Tomislav, Wahl, William, Walkowicz, Lucianne, Walsh, Brian, Walter, Christopher W., Wang, Daniel L., Wang, Shin-Yawn, Warner, Michael, Wiecha, Oliver, Willman, Beth, Winters, Scott E., Wittman, David, Wolff, Sidney C., Wood-Vasey, W. Michael, Wu, Xiuqin, Xin, Bo, Yoachim, Peter, Zhan, Hu, Ivezić, Željko, Kahn, Steven M., Tyson, J. Anthony, Abel, Bob, Acosta, Emily, Allsman, Robyn, Alonso, David, AlSayyad, Yusra, Anderson, Scott F., Andrew, John, Angel, James Roger P., Angeli, George Z., Ansari, Reza, Antilogus, Pierre, Araujo, Constanza, Armstrong, Robert, Arndt, Kirk T., Astier, Pierre, Aubourg, Éric, Auza, Nicole, Axelrod, Tim S., Bard, Deborah J., Barr, Jeff D., Barrau, Aurelian, Bartlett, James G., Bauer, Amanda E., Bauman, Brian J., Baumont, Sylvain, Becker, Andrew C., Becla, Jacek, Beldica, Cristina, Bellavia, Steve, Bianco, Federica B., Biswas, Rahul, Blanc, Guillaume, Blazek, Jonathan, Blandford, Roger D., Bloom, Josh S., Bogart, Joanne, Bond, Tim W., Borgland, Anders W., Borne, Kirk, Bosch, James F., Boutigny, Dominique, Brackett, Craig A., Bradshaw, Andrew, Brandt, William Nielsen, Brown, Michael E., Bullock, James S., Burchat, Patricia, Burke, David L., Cagnoli, Gianpietro, Calabrese, Daniel, Callahan, Shawn, Callen, Alice L., Chandrasekharan, Srinivasan, Charles-Emerson, Glenaver, Chesley, Steve, Cheu, Elliott C., Chiang, Hsin-Fang, Chiang, James, Chirino, Carol, Chow, Derek, Ciardi, David R., Claver, Charles F., Cohen-Tanugi, Johann, Cockrum, Joseph J., Coles, Rebecca, Connolly, Andrew J., Cook, Kem H., Cooray, Asantha, Covey, Kevin R., Cribbs, Chris, Cui, Wei, Cutri, Roc, Daly, Philip N., Daniel, Scott F., Daruich, Felipe, Daubard, Guillaume, Daues, Greg, Dawson, William, Delgado, Francisco, Dellapenna, Alfred, de Peyster, Robert, de Val-Borro, Miguel, Digel, Seth W., Doherty, Peter, Dubois, Richard, Dubois-Felsmann, Gregory P., Durech, Josef, Economou, Frossie, Eracleous, Michael, Ferguson, Henry, Figueroa, Enrique, Fisher-Levine, Merlin, Focke, Warren, Foss, Michael D., Frank, James, Freemon, Michael D., Gangler, Emmanuel, Gawiser, Eric, Geary, John C., Gee, Perry, Geha, Marla, Gessner, Charles J. B., Gibson, Robert R., Gilmore, D. Kirk, Glanzman, Thomas, Glick, William, Goldina, Tatiana, Goldstein, Daniel A., Goodenow, Iain, Graham, Melissa L., Gressler, William J., Gris, Philippe, Guy, Leanne P., Guyonnet, Augustin, Haller, Gunther, Harris, Ron, Hascall, Patrick A., Haupt, Justine, Hernandez, Fabio, Herrmann, Sven, Hileman, Edward, Hoblitt, Joshua, Hodgson, John A., Hogan, Craig, Huang, Dajun, Huffer, Michael E., Ingraham, Patrick, Innes, Walter R., Jacoby, Suzanne H., Jain, Bhuvnesh, Jammes, Fabrice, Jee, James, Jenness, Tim, Jernigan, Garrett, Jevremović, Darko, Johns, Kenneth, Johnson, Anthony S., Johnson, Margaret W. G., Jones, R. Lynne, Juramy-Gilles, Claire, Jurić, Mario, Kalirai, Jason S., Kallivayalil, Nitya J., Kalmbach, Bryce, Kantor, Jeffrey P., Karst, Pierre, Kasliwal, Mansi M., Kelly, Heather, Kessler, Richard, Kinnison, Veronica, Kirkby, David, Knox, Lloyd, Kotov, Ivan V., Krabbendam, Victor L., Krughoff, K. Simon, Kubánek, Petr, Kuczewski, John, Kulkarni, Shri, Ku, John, Kurita, Nadine R., Lage, Craig S., Lambert, Ron, Lange, Travis, Langton, J. Brian, Guillou, Laurent Le, Levine, Deborah, Liang, Ming, Lim, Kian-Tat, Lintott, Chris J., Long, Kevin E., Lopez, Margaux, Lotz, Paul J., Lupton, Robert H., Lust, Nate B., MacArthur, Lauren A., Mahabal, Ashish, Mandelbaum, Rachel, Marsh, Darren S., Marshall, Philip J., Marshall, Stuart, May, Morgan, McKercher, Robert, McQueen, Michelle, Meyers, Joshua, Migliore, Myriam, Miller, Michelle, Mills, David J., Miraval, Connor, Moeyens, Joachim, Monet, David G., Moniez, Marc, Monkewitz, Serge, Montgomery, Christopher, Mueller, Fritz, Muller, Gary P., Arancibia, Freddy Muñoz, Neill, Douglas R., Newbry, Scott P., Nief, Jean-Yves, Nomerotski, Andrei, Nordby, Martin, O'Connor, Paul, Oliver, John, Olivier, Scot S., Olsen, Knut, O'Mullane, William, Ortiz, Sandra, Osier, Shawn, Owen, Russell E., Pain, Reynald, Palecek, Paul E., Parejko, John K., Parsons, James B., Pease, Nathan M., Peterson, J. Matt, Peterson, John R., Petravick, Donald L., Petrick, M. E. Libby, Petry, Cathy E., Pierfederici, Francesco, Pietrowicz, Stephen, Pike, Rob, Pinto, Philip A., Plante, Raymond, Plate, Stephen, Price, Paul A., Prouza, Michael, Radeka, Veljko, Rajagopal, Jayadev, Rasmussen, Andrew P., Regnault, Nicolas, Reil, Kevin A., Reiss, David J., Reuter, Michael A., Ridgway, Stephen T., Riot, Vincent J., Ritz, Steve, Robinson, Sean, Roby, William, Roodman, Aaron, Rosing, Wayne, Roucelle, Cecille, Rumore, Matthew R., Russo, Stefano, Saha, Abhijit, Sassolas, Benoit, Schalk, Terry L., Schellart, Pim, Schindler, Rafe H., Schmidt, Samuel, Schneider, Donald P., Schneider, Michael D., Schoening, William, Schumacher, German, Schwamb, Megan E., Sebag, Jacques, Selvy, Brian, Sembroski, Glenn H., Seppala, Lynn G., Serio, Andrew, Serrano, Eduardo, Shaw, Richard A., Shipsey, Ian, Sick, Jonathan, Silvestri, Nicole, Slater, Colin T., Smith, J. Allyn, Smith, R. Chris, Sobhani, Shahram, Soldahl, Christine, Storrie-Lombardi, Lisa, Stover, Edward, Strauss, Michael A., Street, Rachel A., Stubbs, Christopher W., Sullivan, Ian S., Sweeney, Donald, Swinbank, John D., Szalay, Alexander, Takacs, Peter, Tether, Stephen A., Thaler, Jon J., Thayer, John Gregg, Thomas, Sandrine, Thukral, Vaikunth, Tice, Jeffrey, Trilling, David E., Turri, Max, Van Berg, Richard, Berk, Daniel Vanden, Vetter, Kurt, Virieux, Francoise, Vucina, Tomislav, Wahl, William, Walkowicz, Lucianne, Walsh, Brian, Walter, Christopher W., Wang, Daniel L., Wang, Shin-Yawn, Warner, Michael, Wiecha, Oliver, Willman, Beth, Winters, Scott E., Wittman, David, Wolff, Sidney C., Wood-Vasey, W. Michael, Wu, Xiuqin, Xin, Bo, Yoachim, Peter, and Zhan, Hu
Abstract: (Abridged) We describe here the most ambitious survey currently planned in the optical, the Large Synoptic Survey Telescope (LSST). A vast array of science will be enabled by a single wide-deep-fast sky survey, and LSST will have unique survey capability in the faint time domain. The LSST design is driven by four main science themes: probing dark energy and dark matter, taking an inventory of the Solar System, exploring the transient optical sky, and mapping the Milky Way. LSST will be a wide-field ground-based system sited at Cerro Pach\'{o}n in northern Chile. The telescope will have an 8.4 m (6.5 m effective) primary mirror, a 9.6 deg$^2$ field of view, and a 3.2 Gigapixel camera. The standard observing sequence will consist of pairs of 15-second exposures in a given field, with two such visits in each pointing in a given night. With these repeats, the LSST system is capable of imaging about 10,000 square degrees of sky in a single filter in three nights. The typical 5$\sigma$ point-source depth in a single visit in $r$ will be $\sim 24.5$ (AB). The project is in the construction phase and will begin regular survey operations by 2022. The survey area will be contained within 30,000 deg$^2$ with $\delta<+34.5^\circ$, and will be imaged multiple times in six bands, $ugrizy$, covering the wavelength range 320--1050 nm. About 90\% of the observing time will be devoted to a deep-wide-fast survey mode which will uniformly observe a 18,000 deg$^2$ region about 800 times (summed over all six bands) during the anticipated 10 years of operations, and yield a coadded map to $r\sim27.5$. The remaining 10\% of the observing time will be allocated to projects such as a Very Deep and Fast time domain survey. The goal is to make LSST data products, including a relational database of about 32 trillion observations of 40 billion objects, available to the public and scientists around the world., Comment: 57 pages, 32 color figures, version with high-resolution figures available from https://www.lsst.org/overview
Published: 2008
Full Text: View/download PDF

25. Supernova Shock Breakout from a Red Supergiant

Author: Schawinski, Kevin, Justham, Stephen, Wolf, Christian, Podsiadlowski, Philipp, Sullivan, Mark, Steenbrugge, Katrien C., Bell, Tony, Roeser, Hermann-Josef, Walker, Emma, Astier, Pierre, Balam, Dave, Balland, Christophe, Carlberg, Ray, Conley, Alex, Fouchez, Dominque, Guy, Julien, Hardin, Delphine, Hook, Isobel, Howell, Andy, Pain, Reynald, Perrett, Kathy, Pritchet, Chris, Regnault, Nicolas, Yi, Sukyoung K., Schawinski, Kevin, Justham, Stephen, Wolf, Christian, Podsiadlowski, Philipp, Sullivan, Mark, Steenbrugge, Katrien C., Bell, Tony, Roeser, Hermann-Josef, Walker, Emma, Astier, Pierre, Balam, Dave, Balland, Christophe, Carlberg, Ray, Conley, Alex, Fouchez, Dominque, Guy, Julien, Hardin, Delphine, Hook, Isobel, Howell, Andy, Pain, Reynald, Perrett, Kathy, Pritchet, Chris, Regnault, Nicolas, and Yi, Sukyoung K.
Abstract: Massive stars undergo a violent death when the supply of nuclear fuel in their cores is exhausted, resulting in a catastrophic "core-collapse" supernova. Such events are usually only detected at least a few days after the star has exploded. Observations of the supernova SNLS-04D2dc with the Galaxy Evolution Explorer space telescope reveal a radiative precursor from the supernova shock before the shock reached the surface of the star and show the initial expansion of the star at the beginning of the explosion. Theoretical models of the ultraviolet light curve confirm that the progenitor was a red supergiant, as expected for this type of supernova. These observations provide a way to probe the physics of core-collapse supernovae and the internal structures of their progenitor stars, Comment: Science, in press. 32 pages, 7 figures
Published: 2008
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26. Towards a Cosmological Hubble Diagram for Type II-P Supernovae

Author: Nugent, Peter, Nugent, Peter, Sullivan, Mark, Ellis, Richard, Gal-Yam, Avishay, Leonard, Douglas C., Howell, D. Andrew, Astier, Pierre, Carlberg, Raymond G., Conley, Alex, Fabbro, Sebastien, Fouchez, Dominique, Neill, James D., Pain, Reynald, Perrett, Kathy, Pritchet, Chris J, Regnault, Nicolas, Nugent, Peter, Nugent, Peter, Sullivan, Mark, Ellis, Richard, Gal-Yam, Avishay, Leonard, Douglas C., Howell, D. Andrew, Astier, Pierre, Carlberg, Raymond G., Conley, Alex, Fabbro, Sebastien, Fouchez, Dominique, Neill, James D., Pain, Reynald, Perrett, Kathy, Pritchet, Chris J, and Regnault, Nicolas
Abstract: We present the first high-redshift Hubble diagram for Type II-P supernovae (SNe II-P) based upon five events at redshift up toz~;0.3. This diagram was constructed using photometry from the Canada-France-Hawaii Telescope Supernova Legacy Survey and absorption line spectroscopy from the Keck observatory. The method used to measure distances to these supernovae is based on recent work by Hamuy& Pinto (2002) and exploits a correlation between the absolute brightness of SNe II-P and the expansion velocities derived from the minimum of the Fe II 516.9 nm P-Cygni feature observed during the plateau phases. We present three refinements to this method which significantly improve the practicality of measuring the distances ofSNe II-P at cosmologically interesting redshifts. These are an extinction correction measurement based on the V-I colors at day 50, across-correlation measurement for the expansion velocity and theability to extrapolate such velocities accurately over almost the entire plateau phase. We apply this revised method to our dataset of high-redshift SNe II-P and find that the resulting Hubble diagram hasa scatter of only 0.26 magnitudes, thus demonstrating the feasibility of measuring the expansion history, with present facilities, using amethod independent of that based upon supernovae of Type Ia.
Published: 2006

27. The type Ia supernova SNLS-03D3bb from a super-Chandrasekhar-mass white dwarf star

Author: Howell, D. Andrew, Sullivan, Mark, Nugent, Peter E., Ellis, Richard S., Conley, Alexander J., Borgne, Damien Le, Carlberg, Raymond G., Guy, Julien, Balam, David, Basa, Stephane, Fouchez, Dominique, Hook, Isobel M., Hsiao, Eric Y., Neill, James D., Pain, Reynald, Perrett, Kathryn M., Pritchet, Christopher J., Howell, D. Andrew, Sullivan, Mark, Nugent, Peter E., Ellis, Richard S., Conley, Alexander J., Borgne, Damien Le, Carlberg, Raymond G., Guy, Julien, Balam, David, Basa, Stephane, Fouchez, Dominique, Hook, Isobel M., Hsiao, Eric Y., Neill, James D., Pain, Reynald, Perrett, Kathryn M., and Pritchet, Christopher J.
Abstract: The acceleration of the expansion of the universe, and the need for Dark Energy, were inferred from the observations of Type Ia supernovae (SNe Ia). There is consensus that SNe Ia are thermonuclear explosions that destroy carbon-oxygen white dwarf stars that accrete matter from a companion star, although the nature of this companion remains uncertain. SNe Ia are thought to be reliable distance indicators because they have a standard amount of fuel and a uniform trigger -- they are predicted to explode when the mass of the white dwarf nears the Chandrasekhar mass -- 1.4 solar masses. Here we show that the high redshift supernova SNLS-03D3bb has an exceptionally high luminosity and low kinetic energy that both imply a super-Chandrasekhar mass progenitor. Super-Chandrasekhar mass SNe Ia should preferentially occur in a young stellar population, so this may provide an explanation for the observed trend that overluminous SNe Ia only occur in young environments. Since this supernova does not obey the relations that allow them to be calibrated as standard candles, and since no counterparts have been found at low redshift, future cosmology studies will have to consider contamination from such events., Comment: 9 pages, 4 figures. To appear in Nature Sept. 21. Accompanying News & Views in same issue. Supplementary information available at www.nature.com/nature
Published: 2006
Full Text: View/download PDF

28. Determination of the Hubble constant, the intrinsic scatter of luminosities of Type Ia SNe, and evidence for non-standard dust in other galaxies

Author: Wang, Xiaofeng, Wang, Lifan, Pain, Reynald, Zhou, Xu, Li, Zongwei, Wang, Xiaofeng, Wang, Lifan, Pain, Reynald, Zhou, Xu, and Li, Zongwei
Abstract: A sample of 109 type Ia supernovae (SNe Ia) with recession velocity < 30,000 km s^{-1}, is compiled from published SNe Ia light curves to explore the expansion rate of the local Universe. Based on the color parameter delta C_{12} and the decline rate delta m_{15}, we found that the average absorption to reddening ratio for SN Ia host galaxies to be R_{UBVI} = 4.37+/-0.25, 3.33+/-0.11, 2.30+/-0.11, 1.18+/-0.11, which are systematically lower than the standard values in the Milky Way. We investigated the correlations of the intrinsic luminosity with light curve decline rate, color index, and supernova environmental parameters. In particular, we found SNe Ia in E/S0 galaxies to be brighter close to the central region than those in the outer region, which may suggest a possible metallicity effect on SN luminosity. The dependence of SN luminosity on galactic environment disappears after corrections for the extinction and delta C_{12}. The Hubble diagrams constructed using 73 Hubble flow SNe Ia yield a 1-sigma scatter of <0.12 mag in BVI bands and ~0.16 mag in U band. The luminosity difference between normal SNe Ia and peculiar objects (including SN 1991bg-like and 1991T-like events) has now been reduced to within 0.15 mag via delta C_{12} correction. We use the same precepts to correct the nearby SNe Ia with Cepheid distances and found that the fully corrected absolute magnitudes of SNe Ia are: M_{B} = -19.33+/-0.06 mag, M_{V} = -19.27+/-0.05 mag. We deduced a value for the Hubble constant of H_{0} = 72 +/- 6 (total) km s^{-1} Mpc^{-1}., Comment: 40 pages, 9 figures, ApJ in press
Published: 2006
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29. Towards a Cosmological Hubble Diagram for Type II-P Supernovae

Author: Nugent, Peter, Sullivan, Mark, Ellis, Richard, Gal-Yam, Avishay, Leonard, Douglas C., Howell, D. Andrew, Astier, Pierre, Carlberg, Raymond G., Conley, Alex, Fabbro, Sebastien, Fouchez, Dominique, Neill, James D., Pain, Reynald, Perrett, Kathy, Pritchet, Chris J., Regnault, Nicolas, Nugent, Peter, Sullivan, Mark, Ellis, Richard, Gal-Yam, Avishay, Leonard, Douglas C., Howell, D. Andrew, Astier, Pierre, Carlberg, Raymond G., Conley, Alex, Fabbro, Sebastien, Fouchez, Dominique, Neill, James D., Pain, Reynald, Perrett, Kathy, Pritchet, Chris J., and Regnault, Nicolas
Abstract: We present the first high-redshift Hubble diagram for Type II-P supernovae (SNe II-P) based upon five events at redshift up to z~0.3. This diagram was constructed using photometry from the Canada-France-Hawaii Telescope Supernova Legacy Survey and absorption line spectroscopy from the Keck observatory. The method used to measure distances to these supernovae is based on recent work by Hamuy & Pinto (2002) and exploits a correlation between the absolute brightness of SNe II-P and the expansion velocities derived from the minimum of the Fe II 516.9 nm P-Cygni feature observed during the plateau phases. We present three refinements to this method which significantly improve the practicality of measuring the distances of SNe II-P at cosmologically interesting redshifts. These are an extinction correction measurement based on the V-I colors at day 50, a cross-correlation measurement for the expansion velocity and the ability to extrapolate such velocities accurately over almost the entire plateau phase. We apply this revised method to our dataset of high-redshift SNe II-P and find that the resulting Hubble diagram has a scatter of only 0.26 magnitudes, thus demonstrating the feasibility of measuring the expansion history, with present facilities, using a method independent of that based upon supernovae of Type Ia., Comment: 36 pages, 16 figures, accepted for publication in ApJ
Published: 2006
Full Text: View/download PDF

30. Towards a Cosmological Hubble Diagram for Type II-P Supernovae

Author: Nugent, Peter, Nugent, Peter, Sullivan, Mark, Ellis, Richard, Gal-Yam, Avishay, Leonard, Douglas C., Howell, D. Andrew, Astier, Pierre, Carlberg, Raymond G., Conley, Alex, Fabbro, Sebastien, Fouchez, Dominique, Neill, James D., Pain, Reynald, Perrett, Kathy, Pritchet, Chris J, Regnault, Nicolas, Nugent, Peter, Nugent, Peter, Sullivan, Mark, Ellis, Richard, Gal-Yam, Avishay, Leonard, Douglas C., Howell, D. Andrew, Astier, Pierre, Carlberg, Raymond G., Conley, Alex, Fabbro, Sebastien, Fouchez, Dominique, Neill, James D., Pain, Reynald, Perrett, Kathy, Pritchet, Chris J, and Regnault, Nicolas
Abstract: We present the first high-redshift Hubble diagram for Type II-P supernovae (SNe II-P) based upon five events at redshift up toz~;0.3. This diagram was constructed using photometry from the Canada-France-Hawaii Telescope Supernova Legacy Survey and absorption line spectroscopy from the Keck observatory. The method used to measure distances to these supernovae is based on recent work by Hamuy& Pinto (2002) and exploits a correlation between the absolute brightness of SNe II-P and the expansion velocities derived from the minimum of the Fe II 516.9 nm P-Cygni feature observed during the plateau phases. We present three refinements to this method which significantly improve the practicality of measuring the distances ofSNe II-P at cosmologically interesting redshifts. These are an extinction correction measurement based on the V-I colors at day 50, across-correlation measurement for the expansion velocity and theability to extrapolate such velocities accurately over almost the entire plateau phase. We apply this revised method to our dataset of high-redshift SNe II-P and find that the resulting Hubble diagram hasa scatter of only 0.26 magnitudes, thus demonstrating the feasibility of measuring the expansion history, with present facilities, using amethod independent of that based upon supernovae of Type Ia.
Published: 2006

31. The type Ia supernova SNLS-03D3bb from a super-Chandrasekhar-mass white dwarf star

Author: Howell, D. Andrew, Sullivan, Mark, Nugent, Peter E., Ellis, Richard S., Conley, Alexander J., Borgne, Damien Le, Carlberg, Raymond G., Guy, Julien, Balam, David, Basa, Stephane, Fouchez, Dominique, Hook, Isobel M., Hsiao, Eric Y., Neill, James D., Pain, Reynald, Perrett, Kathryn M., Pritchet, Christopher J., Howell, D. Andrew, Sullivan, Mark, Nugent, Peter E., Ellis, Richard S., Conley, Alexander J., Borgne, Damien Le, Carlberg, Raymond G., Guy, Julien, Balam, David, Basa, Stephane, Fouchez, Dominique, Hook, Isobel M., Hsiao, Eric Y., Neill, James D., Pain, Reynald, Perrett, Kathryn M., and Pritchet, Christopher J.
Abstract: The acceleration of the expansion of the universe, and the need for Dark Energy, were inferred from the observations of Type Ia supernovae (SNe Ia). There is consensus that SNe Ia are thermonuclear explosions that destroy carbon-oxygen white dwarf stars that accrete matter from a companion star, although the nature of this companion remains uncertain. SNe Ia are thought to be reliable distance indicators because they have a standard amount of fuel and a uniform trigger -- they are predicted to explode when the mass of the white dwarf nears the Chandrasekhar mass -- 1.4 solar masses. Here we show that the high redshift supernova SNLS-03D3bb has an exceptionally high luminosity and low kinetic energy that both imply a super-Chandrasekhar mass progenitor. Super-Chandrasekhar mass SNe Ia should preferentially occur in a young stellar population, so this may provide an explanation for the observed trend that overluminous SNe Ia only occur in young environments. Since this supernova does not obey the relations that allow them to be calibrated as standard candles, and since no counterparts have been found at low redshift, future cosmology studies will have to consider contamination from such events., Comment: 9 pages, 4 figures. To appear in Nature Sept. 21. Accompanying News & Views in same issue. Supplementary information available at www.nature.com/nature
Published: 2006
Full Text: View/download PDF

32. Towards a Cosmological Hubble Diagram for Type II-P Supernovae

Author: Nugent, Peter, Sullivan, Mark, Ellis, Richard, Gal-Yam, Avishay, Leonard, Douglas C., Howell, D. Andrew, Astier, Pierre, Carlberg, Raymond G., Conley, Alex, Fabbro, Sebastien, Fouchez, Dominique, Neill, James D., Pain, Reynald, Perrett, Kathy, Pritchet, Chris J., Regnault, Nicolas, Nugent, Peter, Sullivan, Mark, Ellis, Richard, Gal-Yam, Avishay, Leonard, Douglas C., Howell, D. Andrew, Astier, Pierre, Carlberg, Raymond G., Conley, Alex, Fabbro, Sebastien, Fouchez, Dominique, Neill, James D., Pain, Reynald, Perrett, Kathy, Pritchet, Chris J., and Regnault, Nicolas
Abstract: We present the first high-redshift Hubble diagram for Type II-P supernovae (SNe II-P) based upon five events at redshift up to z~0.3. This diagram was constructed using photometry from the Canada-France-Hawaii Telescope Supernova Legacy Survey and absorption line spectroscopy from the Keck observatory. The method used to measure distances to these supernovae is based on recent work by Hamuy & Pinto (2002) and exploits a correlation between the absolute brightness of SNe II-P and the expansion velocities derived from the minimum of the Fe II 516.9 nm P-Cygni feature observed during the plateau phases. We present three refinements to this method which significantly improve the practicality of measuring the distances of SNe II-P at cosmologically interesting redshifts. These are an extinction correction measurement based on the V-I colors at day 50, a cross-correlation measurement for the expansion velocity and the ability to extrapolate such velocities accurately over almost the entire plateau phase. We apply this revised method to our dataset of high-redshift SNe II-P and find that the resulting Hubble diagram has a scatter of only 0.26 magnitudes, thus demonstrating the feasibility of measuring the expansion history, with present facilities, using a method independent of that based upon supernovae of Type Ia., Comment: 36 pages, 16 figures, accepted for publication in ApJ
Published: 2006
Full Text: View/download PDF

33. Determination of the Hubble constant, the intrinsic scatter of luminosities of Type Ia SNe, and evidence for non-standard dust in other galaxies

Author: Wang, Xiaofeng, Wang, Lifan, Pain, Reynald, Zhou, Xu, Li, Zongwei, Wang, Xiaofeng, Wang, Lifan, Pain, Reynald, Zhou, Xu, and Li, Zongwei
Abstract: A sample of 109 type Ia supernovae (SNe Ia) with recession velocity < 30,000 km s^{-1}, is compiled from published SNe Ia light curves to explore the expansion rate of the local Universe. Based on the color parameter delta C_{12} and the decline rate delta m_{15}, we found that the average absorption to reddening ratio for SN Ia host galaxies to be R_{UBVI} = 4.37+/-0.25, 3.33+/-0.11, 2.30+/-0.11, 1.18+/-0.11, which are systematically lower than the standard values in the Milky Way. We investigated the correlations of the intrinsic luminosity with light curve decline rate, color index, and supernova environmental parameters. In particular, we found SNe Ia in E/S0 galaxies to be brighter close to the central region than those in the outer region, which may suggest a possible metallicity effect on SN luminosity. The dependence of SN luminosity on galactic environment disappears after corrections for the extinction and delta C_{12}. The Hubble diagrams constructed using 73 Hubble flow SNe Ia yield a 1-sigma scatter of <0.12 mag in BVI bands and ~0.16 mag in U band. The luminosity difference between normal SNe Ia and peculiar objects (including SN 1991bg-like and 1991T-like events) has now been reduced to within 0.15 mag via delta C_{12} correction. We use the same precepts to correct the nearby SNe Ia with Cepheid distances and found that the fully corrected absolute magnitudes of SNe Ia are: M_{B} = -19.33+/-0.06 mag, M_{V} = -19.27+/-0.05 mag. We deduced a value for the Hubble constant of H_{0} = 72 +/- 6 (total) km s^{-1} Mpc^{-1}., Comment: 40 pages, 9 figures, ApJ in press
Published: 2006
Full Text: View/download PDF

34. Overview of the nearby supernova factory

Author: Aldering, Greg, Aldering, Greg, Adam, Gilles, Antilogus, Pierre, Astier, Pierre, Bacon, Roland, Bongard, S., Bonnaud, C., Copin, Yannick, Hardin, D., Howell, D. Andy, Lemmonnier, Jean-Pierre, Levy, J.-M., Loken, S., Nugent, Peter, Pain, Reynald, Pecontal, Arlette, Pecontal, Emmanuel, Perlmutter, Saul, Quimby, Robert, Schahmaneche, Kyan, Smadja, Gerard, Wood-Vasey, W. Michael, Aldering, Greg, Aldering, Greg, Adam, Gilles, Antilogus, Pierre, Astier, Pierre, Bacon, Roland, Bongard, S., Bonnaud, C., Copin, Yannick, Hardin, D., Howell, D. Andy, Lemmonnier, Jean-Pierre, Levy, J.-M., Loken, S., Nugent, Peter, Pain, Reynald, Pecontal, Arlette, Pecontal, Emmanuel, Perlmutter, Saul, Quimby, Robert, Schahmaneche, Kyan, Smadja, Gerard, and Wood-Vasey, W. Michael
Published: 2002

35. Overview of the nearby supernova factory

Author: Aldering, Greg, Aldering, Greg, Adam, Gilles, Antilogus, Pierre, Astier, Pierre, Bacon, Roland, Bongard, S., Bonnaud, C., Copin, Yannick, Hardin, D., Howell, D. Andy, Lemmonnier, Jean-Pierre, Levy, J.-M., Loken, S., Nugent, Peter, Pain, Reynald, Pecontal, Arlette, Pecontal, Emmanuel, Perlmutter, Saul, Quimby, Robert, Schahmaneche, Kyan, Smadja, Gerard, Wood-Vasey, W. Michael, Aldering, Greg, Aldering, Greg, Adam, Gilles, Antilogus, Pierre, Astier, Pierre, Bacon, Roland, Bongard, S., Bonnaud, C., Copin, Yannick, Hardin, D., Howell, D. Andy, Lemmonnier, Jean-Pierre, Levy, J.-M., Loken, S., Nugent, Peter, Pain, Reynald, Pecontal, Arlette, Pecontal, Emmanuel, Perlmutter, Saul, Quimby, Robert, Schahmaneche, Kyan, Smadja, Gerard, and Wood-Vasey, W. Michael
Published: 2002

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35 results on '"Pain, Reynald"'

1. The HST See Change Program. I. Survey Design, Pipeline, and Supernova Discoveries

2. The HST See Change Program: I. Survey Design, Pipeline, and Supernova Discoveries

3. The HST See Change Program. I. Survey Design, Pipeline, and Supernova Discoveries

4. High-Redshift SNe with Subaru and HST

5. The Discovery of a Gravitationally Lensed Supernova Ia at Redshift 2.22

6. The Discovery of a Gravitationally Lensed Supernova Ia at Redshift 2.22

7. The Discovery of a Gravitationally Lensed Supernova Ia at Redshift 2.22

8. The Discovery of a Gravitationally Lensed Supernova Ia at Redshift 2.22

9. RAPIDLY RISING TRANSIENTS IN THE SUPERNOVA-SUPERLUMINOUS SUPERNOVA GAP

10. Rapidly Rising Transients in the Supernova - Superluminous Supernova Gap

11. Rapidly Rising Transients in the Supernova - Superluminous Supernova Gap

12. The Type Ia supernovae rate with Subaru/XMM-Newton Deep Survey

13. The Type Ia supernovae rate with Subaru/XMM-Newton Deep Survey

14. The Type Ia supernovae rate with Subaru/XMM-Newton Deep Survey

15. Observational Evidence of the Accelerated Expansion of the Universe

16. Observational Evidence of the Accelerated Expansion of the Universe

17. Subaru FOCAS Spectroscopic Observations of High-Redshift Supernovae

18. Subaru FOCAS Spectroscopic Observations of High-Redshift Supernovae

19. Subaru FOCAS Spectroscopic Observations of High-Redshift Supernovae

20. The type Ia supernova SNLS-03D3bb from a super-Chandrasekhar-mass white dwarf star

21. LSST: from Science Drivers to Reference Design and Anticipated Data Products

22. Supernova Shock Breakout from a Red Supergiant

23. The type Ia supernova SNLS-03D3bb from a super-Chandrasekhar-mass white dwarf star

24. LSST: from Science Drivers to Reference Design and Anticipated Data Products

25. Supernova Shock Breakout from a Red Supergiant

26. Towards a Cosmological Hubble Diagram for Type II-P Supernovae

27. The type Ia supernova SNLS-03D3bb from a super-Chandrasekhar-mass white dwarf star

28. Determination of the Hubble constant, the intrinsic scatter of luminosities of Type Ia SNe, and evidence for non-standard dust in other galaxies

29. Towards a Cosmological Hubble Diagram for Type II-P Supernovae

30. Towards a Cosmological Hubble Diagram for Type II-P Supernovae

31. The type Ia supernova SNLS-03D3bb from a super-Chandrasekhar-mass white dwarf star

32. Towards a Cosmological Hubble Diagram for Type II-P Supernovae

33. Determination of the Hubble constant, the intrinsic scatter of luminosities of Type Ia SNe, and evidence for non-standard dust in other galaxies

34. Overview of the nearby supernova factory

35. Overview of the nearby supernova factory

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35 results on '"Pain, Reynald"'

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