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1. DES16C3cje: A low-luminosity, long-lived supernova

Author

Gutiérrez, CP, Gutiérrez, CP, Sullivan, M, Martinez, L, Bersten, MC, Inserra, C, Smith, M, Anderson, JP, Pan, YC, Pastorello, A, Galbany, L, Nugent, P, Angus, CR, Barbarino, C, Carollo, D, Chen, TW, Davis, TM, Della Valle, M, Foley, RJ, Fraser, M, Frohmaier, C, González-Gaitán, S, Gromadzki, M, Kankare, E, Kokotanekova, R, Kollmeier, J, Lewis, GF, Magee, MR, Maguire, K, Möller, A, Morrell, N, Nicholl, M, Pursiainen, M, Sollerman, J, Sommer, NE, Swann, E, Tucker, BE, Wiseman, P, Aguena, M, Allam, S, Avila, S, Bertin, E, Brooks, D, Buckley-Geer, E, Burke, DL, Carnero Rosell, A, Carrasco Kind, M, Carretero, J, Costanzi, M, Da Costa, LN, De Vicente, J, Desai, S, Diehl, HT, Doel, P, Eifler, TF, Flaugher, B, Fosalba, P, Frieman, J, García-Bellido, J, Gerdes, DW, Gruen, D, Gruendl, RA, Gschwend, J, Gutierrez, G, Hinton, SR, Hollowood, DL, Honscheid, K, James, DJ, Kuehn, K, Kuropatkin, N, Lahav, O, Lima, M, Maia, MAG, March, M, Menanteau, F, Miquel, R, Morganson, E, Palmese, A, Paz-Chinchón, F, Plazas, AA, Sako, M, Sanchez, E, Scarpine, V, Schubnell, M, Serrano, S, Sevilla-Noarbe, I, Soares-Santos, M, Suchyta, E, Swanson, MEC, Tarle, G, Thomas, D, Varga, TN, Walker, AR, Wilkinson, R, Gutiérrez, CP, Gutiérrez, CP, Sullivan, M, Martinez, L, Bersten, MC, Inserra, C, Smith, M, Anderson, JP, Pan, YC, Pastorello, A, Galbany, L, Nugent, P, Angus, CR, Barbarino, C, Carollo, D, Chen, TW, Davis, TM, Della Valle, M, Foley, RJ, Fraser, M, Frohmaier, C, González-Gaitán, S, Gromadzki, M, Kankare, E, Kokotanekova, R, Kollmeier, J, Lewis, GF, Magee, MR, Maguire, K, Möller, A, Morrell, N, Nicholl, M, Pursiainen, M, Sollerman, J, Sommer, NE, Swann, E, Tucker, BE, Wiseman, P, Aguena, M, Allam, S, Avila, S, Bertin, E, Brooks, D, Buckley-Geer, E, Burke, DL, Carnero Rosell, A, Carrasco Kind, M, Carretero, J, Costanzi, M, Da Costa, LN, De Vicente, J, Desai, S, Diehl, HT, Doel, P, Eifler, TF, Flaugher, B, Fosalba, P, Frieman, J, García-Bellido, J, Gerdes, DW, Gruen, D, Gruendl, RA, Gschwend, J, Gutierrez, G, Hinton, SR, Hollowood, DL, Honscheid, K, James, DJ, Kuehn, K, Kuropatkin, N, Lahav, O, Lima, M, Maia, MAG, March, M, Menanteau, F, Miquel, R, Morganson, E, Palmese, A, Paz-Chinchón, F, Plazas, AA, Sako, M, Sanchez, E, Scarpine, V, Schubnell, M, Serrano, S, Sevilla-Noarbe, I, Soares-Santos, M, Suchyta, E, Swanson, MEC, Tarle, G, Thomas, D, Varga, TN, Walker, AR, and Wilkinson, R

Abstract

We present DES16C3cje, a low-luminosity, long-lived type II supernova (SN II) at redshift 0.0618, detected by the Dark Energy Survey (DES). DES16C3cje is a unique SN. The spectra are characterized by extremely narrow photospheric lines corresponding to very low expansion velocities of1500 km s-1, and the light curve shows an initial peak that fades after 50 d before slowly rebrightening over a further 100 d to reach an absolute brightness of Mr ∼-15.5 mag. The decline rate of the late-time light curve is then slower than that expected from the powering by radioactive decay of 56Co, but is comparable to that expected from accretion power. Comparing the bolometric light curve with hydrodynamical models, we find that DES16C3cje can be explained by either (i) a low explosion energy (0.11 foe) and relatively large 56Ni production of 0.075 M· from an ∼15 M· red supergiant progenitor typical of other SNe II, or (ii) a relatively compact ∼40 M· star, explosion energy of 1 foe, and 0.08 M· of 56Ni. Both scenarios require additional energy input to explain the late-time light curve, which is consistent with fallback accretion at a rate of ∼0.5 × 10-8 M· s-1.

Published
2020

2. DES16C3cje: A low-luminosity, long-lived supernova

Author

Gutiérrez, CP, Gutiérrez, CP, Sullivan, M, Martinez, L, Bersten, MC, Inserra, C, Smith, M, Anderson, JP, Pan, YC, Pastorello, A, Galbany, L, Nugent, P, Angus, CR, Barbarino, C, Carollo, D, Chen, TW, Davis, TM, Della Valle, M, Foley, RJ, Fraser, M, Frohmaier, C, González-Gaitán, S, Gromadzki, M, Kankare, E, Kokotanekova, R, Kollmeier, J, Lewis, GF, Magee, MR, Maguire, K, Möller, A, Morrell, N, Nicholl, M, Pursiainen, M, Sollerman, J, Sommer, NE, Swann, E, Tucker, BE, Wiseman, P, Aguena, M, Allam, S, Avila, S, Bertin, E, Brooks, D, Buckley-Geer, E, Burke, DL, Carnero Rosell, A, Carrasco Kind, M, Carretero, J, Costanzi, M, Da Costa, LN, De Vicente, J, Desai, S, Diehl, HT, Doel, P, Eifler, TF, Flaugher, B, Fosalba, P, Frieman, J, García-Bellido, J, Gerdes, DW, Gruen, D, Gruendl, RA, Gschwend, J, Gutierrez, G, Hinton, SR, Hollowood, DL, Honscheid, K, James, DJ, Kuehn, K, Kuropatkin, N, Lahav, O, Lima, M, Maia, MAG, March, M, Menanteau, F, Miquel, R, Morganson, E, Palmese, A, Paz-Chinchón, F, Plazas, AA, Sako, M, Sanchez, E, Scarpine, V, Schubnell, M, Serrano, S, Sevilla-Noarbe, I, Soares-Santos, M, Suchyta, E, Swanson, MEC, Tarle, G, Thomas, D, Varga, TN, Walker, AR, Wilkinson, R, Gutiérrez, CP, Gutiérrez, CP, Sullivan, M, Martinez, L, Bersten, MC, Inserra, C, Smith, M, Anderson, JP, Pan, YC, Pastorello, A, Galbany, L, Nugent, P, Angus, CR, Barbarino, C, Carollo, D, Chen, TW, Davis, TM, Della Valle, M, Foley, RJ, Fraser, M, Frohmaier, C, González-Gaitán, S, Gromadzki, M, Kankare, E, Kokotanekova, R, Kollmeier, J, Lewis, GF, Magee, MR, Maguire, K, Möller, A, Morrell, N, Nicholl, M, Pursiainen, M, Sollerman, J, Sommer, NE, Swann, E, Tucker, BE, Wiseman, P, Aguena, M, Allam, S, Avila, S, Bertin, E, Brooks, D, Buckley-Geer, E, Burke, DL, Carnero Rosell, A, Carrasco Kind, M, Carretero, J, Costanzi, M, Da Costa, LN, De Vicente, J, Desai, S, Diehl, HT, Doel, P, Eifler, TF, Flaugher, B, Fosalba, P, Frieman, J, García-Bellido, J, Gerdes, DW, Gruen, D, Gruendl, RA, Gschwend, J, Gutierrez, G, Hinton, SR, Hollowood, DL, Honscheid, K, James, DJ, Kuehn, K, Kuropatkin, N, Lahav, O, Lima, M, Maia, MAG, March, M, Menanteau, F, Miquel, R, Morganson, E, Palmese, A, Paz-Chinchón, F, Plazas, AA, Sako, M, Sanchez, E, Scarpine, V, Schubnell, M, Serrano, S, Sevilla-Noarbe, I, Soares-Santos, M, Suchyta, E, Swanson, MEC, Tarle, G, Thomas, D, Varga, TN, Walker, AR, and Wilkinson, R

Abstract

We present DES16C3cje, a low-luminosity, long-lived type II supernova (SN II) at redshift 0.0618, detected by the Dark Energy Survey (DES). DES16C3cje is a unique SN. The spectra are characterized by extremely narrow photospheric lines corresponding to very low expansion velocities of1500 km s-1, and the light curve shows an initial peak that fades after 50 d before slowly rebrightening over a further 100 d to reach an absolute brightness of Mr ∼-15.5 mag. The decline rate of the late-time light curve is then slower than that expected from the powering by radioactive decay of 56Co, but is comparable to that expected from accretion power. Comparing the bolometric light curve with hydrodynamical models, we find that DES16C3cje can be explained by either (i) a low explosion energy (0.11 foe) and relatively large 56Ni production of 0.075 M· from an ∼15 M· red supergiant progenitor typical of other SNe II, or (ii) a relatively compact ∼40 M· star, explosion energy of 1 foe, and 0.08 M· of 56Ni. Both scenarios require additional energy input to explain the late-time light curve, which is consistent with fallback accretion at a rate of ∼0.5 × 10-8 M· s-1.

Published
2020

3. The mystery of photometric twins DES17X1boj and DES16E2bjy

Author

Pursiainen, M, Pursiainen, M, Gutiérrez, CP, Wiseman, P, Childress, M, Smith, M, Frohmaier, C, Angus, C, Castro Segura, N, Kelsey, L, Sullivan, M, Galbany, L, Nugent, P, Bassett, BA, Brout, D, Carollo, D, D'andrea, CB, Davis, TM, Foley, RJ, Grayling, M, Hinton, SR, Inserra, C, Kessler, R, Lewis, GF, Lidman, C, Macaulay, E, March, M, Möller, A, Müller, T, Scolnic, D, Sommer, NE, Swann, E, Thomas, BP, Tucker, BE, Vincenzi, M, Abbott, TMC, Allam, S, Annis, J, Avila, S, Bertin, E, Brooks, D, Buckley-Geer, E, Burke, DL, Carnero Rosell, A, Carrasco Kind, M, Da Costa, LN, De Vicente, J, Desai, S, Diehl, HT, Doel, P, Eifler, TF, Everett, S, Flaugher, B, Frieman, J, García-Bellido, J, Gaztanaga, E, Gerdes, DW, Gruen, D, Gruendl, RA, Gschwend, J, Gutierrez, G, Hollowood, DL, Honscheid, K, James, DJ, Kim, AG, Krause, E, Kuehn, K, Maia, MAG, Marshall, JL, Menanteau, F, Miquel, R, Ogando, RLC, Palmese, A, Paz-Chinchón, F, Plazas, AA, Roodman, A, Sanchez, E, Scarpine, V, Schubnell, M, Serrano, S, Sevilla-Noarbe, I, Suchyta, E, Swanson, MEC, Tarle, G, Wester, W, Pursiainen, M, Pursiainen, M, Gutiérrez, CP, Wiseman, P, Childress, M, Smith, M, Frohmaier, C, Angus, C, Castro Segura, N, Kelsey, L, Sullivan, M, Galbany, L, Nugent, P, Bassett, BA, Brout, D, Carollo, D, D'andrea, CB, Davis, TM, Foley, RJ, Grayling, M, Hinton, SR, Inserra, C, Kessler, R, Lewis, GF, Lidman, C, Macaulay, E, March, M, Möller, A, Müller, T, Scolnic, D, Sommer, NE, Swann, E, Thomas, BP, Tucker, BE, Vincenzi, M, Abbott, TMC, Allam, S, Annis, J, Avila, S, Bertin, E, Brooks, D, Buckley-Geer, E, Burke, DL, Carnero Rosell, A, Carrasco Kind, M, Da Costa, LN, De Vicente, J, Desai, S, Diehl, HT, Doel, P, Eifler, TF, Everett, S, Flaugher, B, Frieman, J, García-Bellido, J, Gaztanaga, E, Gerdes, DW, Gruen, D, Gruendl, RA, Gschwend, J, Gutierrez, G, Hollowood, DL, Honscheid, K, James, DJ, Kim, AG, Krause, E, Kuehn, K, Maia, MAG, Marshall, JL, Menanteau, F, Miquel, R, Ogando, RLC, Palmese, A, Paz-Chinchón, F, Plazas, AA, Roodman, A, Sanchez, E, Scarpine, V, Schubnell, M, Serrano, S, Sevilla-Noarbe, I, Suchyta, E, Swanson, MEC, Tarle, G, and Wester, W

Abstract

We present an analysis of DES17X1boj and DES16E2bjy, two peculiar transients discovered by the Dark Energy Survey (DES). They exhibit nearly identical double-peaked light curves that reach very different maximum luminosities (Mr = -15.4 and -17.9, respectively). The light-curve evolution of these events is highly atypical and has not been reported before. The transients are found in different host environments: DES17X1boj was found near the nucleus of a spiral galaxy, while DES16E2bjy is located in the outskirts of a passive red galaxy. Early photometric data are well fitted with a blackbody and the resulting moderate photospheric expansion velocities (1800 km s-1 for DES17X1boj and 4800 km s-1 for DES16E2bjy) suggest an explosive or eruptive origin. Additionally, a feature identified as high-velocity Ca ii absorption (v ≈ 9400 km s-1) in the near-peak spectrum of DES17X1boj may imply that it is a supernova. While similar light-curve evolution suggests a similar physical origin for these two transients, we are not able to identify or characterize the progenitors.

Published
2020

4. The mystery of photometric twins DES17X1boj and DES16E2bjy

Author

Pursiainen, M, Pursiainen, M, Gutiérrez, CP, Wiseman, P, Childress, M, Smith, M, Frohmaier, C, Angus, C, Castro Segura, N, Kelsey, L, Sullivan, M, Galbany, L, Nugent, P, Bassett, BA, Brout, D, Carollo, D, D'andrea, CB, Davis, TM, Foley, RJ, Grayling, M, Hinton, SR, Inserra, C, Kessler, R, Lewis, GF, Lidman, C, Macaulay, E, March, M, Möller, A, Müller, T, Scolnic, D, Sommer, NE, Swann, E, Thomas, BP, Tucker, BE, Vincenzi, M, Abbott, TMC, Allam, S, Annis, J, Avila, S, Bertin, E, Brooks, D, Buckley-Geer, E, Burke, DL, Carnero Rosell, A, Carrasco Kind, M, Da Costa, LN, De Vicente, J, Desai, S, Diehl, HT, Doel, P, Eifler, TF, Everett, S, Flaugher, B, Frieman, J, García-Bellido, J, Gaztanaga, E, Gerdes, DW, Gruen, D, Gruendl, RA, Gschwend, J, Gutierrez, G, Hollowood, DL, Honscheid, K, James, DJ, Kim, AG, Krause, E, Kuehn, K, Maia, MAG, Marshall, JL, Menanteau, F, Miquel, R, Ogando, RLC, Palmese, A, Paz-Chinchón, F, Plazas, AA, Roodman, A, Sanchez, E, Scarpine, V, Schubnell, M, Serrano, S, Sevilla-Noarbe, I, Suchyta, E, Swanson, MEC, Tarle, G, Wester, W, Pursiainen, M, Pursiainen, M, Gutiérrez, CP, Wiseman, P, Childress, M, Smith, M, Frohmaier, C, Angus, C, Castro Segura, N, Kelsey, L, Sullivan, M, Galbany, L, Nugent, P, Bassett, BA, Brout, D, Carollo, D, D'andrea, CB, Davis, TM, Foley, RJ, Grayling, M, Hinton, SR, Inserra, C, Kessler, R, Lewis, GF, Lidman, C, Macaulay, E, March, M, Möller, A, Müller, T, Scolnic, D, Sommer, NE, Swann, E, Thomas, BP, Tucker, BE, Vincenzi, M, Abbott, TMC, Allam, S, Annis, J, Avila, S, Bertin, E, Brooks, D, Buckley-Geer, E, Burke, DL, Carnero Rosell, A, Carrasco Kind, M, Da Costa, LN, De Vicente, J, Desai, S, Diehl, HT, Doel, P, Eifler, TF, Everett, S, Flaugher, B, Frieman, J, García-Bellido, J, Gaztanaga, E, Gerdes, DW, Gruen, D, Gruendl, RA, Gschwend, J, Gutierrez, G, Hollowood, DL, Honscheid, K, James, DJ, Kim, AG, Krause, E, Kuehn, K, Maia, MAG, Marshall, JL, Menanteau, F, Miquel, R, Ogando, RLC, Palmese, A, Paz-Chinchón, F, Plazas, AA, Roodman, A, Sanchez, E, Scarpine, V, Schubnell, M, Serrano, S, Sevilla-Noarbe, I, Suchyta, E, Swanson, MEC, Tarle, G, and Wester, W

Abstract

We present an analysis of DES17X1boj and DES16E2bjy, two peculiar transients discovered by the Dark Energy Survey (DES). They exhibit nearly identical double-peaked light curves that reach very different maximum luminosities (Mr = -15.4 and -17.9, respectively). The light-curve evolution of these events is highly atypical and has not been reported before. The transients are found in different host environments: DES17X1boj was found near the nucleus of a spiral galaxy, while DES16E2bjy is located in the outskirts of a passive red galaxy. Early photometric data are well fitted with a blackbody and the resulting moderate photospheric expansion velocities (1800 km s-1 for DES17X1boj and 4800 km s-1 for DES16E2bjy) suggest an explosive or eruptive origin. Additionally, a feature identified as high-velocity Ca ii absorption (v ≈ 9400 km s-1) in the near-peak spectrum of DES17X1boj may imply that it is a supernova. While similar light-curve evolution suggests a similar physical origin for these two transients, we are not able to identify or characterize the progenitors.

Published
2020

5. UBVRIz light curves of 51 type II supernovae

Author

Galbany, L, Galbany, L, Hamuy, M, Phillips, MM, Suntzeff, NB, Maza, J, Jaeger, TD, Moraga, T, González-Gaitán, S, Krisciunas, K, Morrell, NI, Thomas-Osip, J, Krzeminski, W, González, L, Antezana, R, Wishnjewski, M, McCarthy, P, Anderson, JP, Gutiérrez, CP, Stritzinger, M, Folatelli, G, Anguita, C, Galaz, G, Green, EM, Impey, C, Kim, YC, Kirhakos, S, Malkan, MA, Mulchaey, JS, Phillips, AC, Pizzella, A, Prosser, CF, Schmidt, BP, Schommer, RA, Sherry, W, Strolger, LG, Wells, LA, Williger, GM, Galbany, L, Galbany, L, Hamuy, M, Phillips, MM, Suntzeff, NB, Maza, J, Jaeger, TD, Moraga, T, González-Gaitán, S, Krisciunas, K, Morrell, NI, Thomas-Osip, J, Krzeminski, W, González, L, Antezana, R, Wishnjewski, M, McCarthy, P, Anderson, JP, Gutiérrez, CP, Stritzinger, M, Folatelli, G, Anguita, C, Galaz, G, Green, EM, Impey, C, Kim, YC, Kirhakos, S, Malkan, MA, Mulchaey, JS, Phillips, AC, Pizzella, A, Prosser, CF, Schmidt, BP, Schommer, RA, Sherry, W, Strolger, LG, Wells, LA, and Williger, GM

Abstract

We present a compilation of UBVRIz light curves of 51 type II supernovae discovered during the course of four different surveys during 1986-2003: the Cerro Tololo Supernova Survey, the Calán/Tololo Supernova Program (C&T), the Supernova Optical and Infrared Survey (SOIRS), and the Carnegie Type II Supernova Survey (CATS). The photometry is based on template-subtracted images to eliminate any potential host galaxy light contamination, and calibrated from foreground stars. This work presents these photometric data, studies the color evolution using different bands, and explores the relation between the magnitude at maximum brightness and the brightness decline parameter (s) from maximum light through the end of the recombination phase. This parameter is found to be shallower for redder bands and appears to have the best correlation in the B band. In addition, it also correlates with the plateau duration, being shorter (longer) for larger (smaller) s values.

Published
2016

6. UBVRIz light curves of 51 type II supernovae

Author

Galbany, L, Galbany, L, Hamuy, M, Phillips, MM, Suntzeff, NB, Maza, J, Jaeger, TD, Moraga, T, González-Gaitán, S, Krisciunas, K, Morrell, NI, Thomas-Osip, J, Krzeminski, W, González, L, Antezana, R, Wishnjewski, M, McCarthy, P, Anderson, JP, Gutiérrez, CP, Stritzinger, M, Folatelli, G, Anguita, C, Galaz, G, Green, EM, Impey, C, Kim, YC, Kirhakos, S, Malkan, MA, Mulchaey, JS, Phillips, AC, Pizzella, A, Prosser, CF, Schmidt, BP, Schommer, RA, Sherry, W, Strolger, LG, Wells, LA, Williger, GM, Galbany, L, Galbany, L, Hamuy, M, Phillips, MM, Suntzeff, NB, Maza, J, Jaeger, TD, Moraga, T, González-Gaitán, S, Krisciunas, K, Morrell, NI, Thomas-Osip, J, Krzeminski, W, González, L, Antezana, R, Wishnjewski, M, McCarthy, P, Anderson, JP, Gutiérrez, CP, Stritzinger, M, Folatelli, G, Anguita, C, Galaz, G, Green, EM, Impey, C, Kim, YC, Kirhakos, S, Malkan, MA, Mulchaey, JS, Phillips, AC, Pizzella, A, Prosser, CF, Schmidt, BP, Schommer, RA, Sherry, W, Strolger, LG, Wells, LA, and Williger, GM

Abstract

We present a compilation of UBVRIz light curves of 51 type II supernovae discovered during the course of four different surveys during 1986-2003: the Cerro Tololo Supernova Survey, the Calán/Tololo Supernova Program (C&T), the Supernova Optical and Infrared Survey (SOIRS), and the Carnegie Type II Supernova Survey (CATS). The photometry is based on template-subtracted images to eliminate any potential host galaxy light contamination, and calibrated from foreground stars. This work presents these photometric data, studies the color evolution using different bands, and explores the relation between the magnitude at maximum brightness and the brightness decline parameter (s) from maximum light through the end of the recombination phase. This parameter is found to be shallower for redder bands and appears to have the best correlation in the B band. In addition, it also correlates with the plateau duration, being shorter (longer) for larger (smaller) s values.

Published
2016

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