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1. Annotated Coadds: Concise Metrics for Characterizing Survey Cadence and for Discovering Variable and Transient Sources

Author

Shupe, D. L., Masci, F. J., Chary, R., Helou, G., Faisst, A. L., Cutri, R. M., Brooke, T. Y., Surace, J. A., Marsh, K. A., Shupe, D. L., Masci, F. J., Chary, R., Helou, G., Faisst, A. L., Cutri, R. M., Brooke, T. Y., Surace, J. A., and Marsh, K. A.

Abstract

In order to study transient phenomena in the Universe, existing and forthcoming imaging surveys are covering wide areas of sky repeatedly over time, with a range of cadences, point spread functions, and depths. We describe here a framework that allows an efficient search for different types of time-varying astrophysical phenomena in current and future, large data repositories. We first present a methodology to generate and store key survey parameters that enable researchers to determine if a survey, or a combination of surveys, allows specific time-variable astrophysical phenomena to be discovered. To facilitate further exploration of sources in regions of interest, we then generate a few sample metrics that capture the essential brightness characteristics of a sky pixel at a specific wavelength. Together, we refer to these as "annotated coadds". The techniques presented here for WISE/NEOWISE-R data are sensitive to 10 percent brightness variations at around 12th Vega magnitude at 4.5 microns wavelength. Application of the technique to ZTF data also enabled the detection of 0.5 mag variability at 20 AB mag in the r-band. We demonstrate the capabilities of these metrics for different classes of sources: high proper-motion stars, periodic variable stars, and supernovae, and find that each metric has its advantages depending on the nature of variability. We also present a data structure which will ease the search for temporally varying phenomena in future surveys., Comment: 26 pages, 11 figures, PASP in press

Published
2023

2. Constraining Type Ia supernova explosions and early flux excesses with the Zwicky Transient Factory

Author

Deckers, M., Maguire, K., Magee, M. R., Dimitriadis, G., Smith, M., Sainz de Murieta, A., Miller, A. A., Goobar, Ariel, Nordin, J., Rigault, M., Bellm, E. C., Coughlin, M., Laher, R. R., Shupe, D. L., Graham, M., Kasliwal, M., Walters, R., Deckers, M., Maguire, K., Magee, M. R., Dimitriadis, G., Smith, M., Sainz de Murieta, A., Miller, A. A., Goobar, Ariel, Nordin, J., Rigault, M., Bellm, E. C., Coughlin, M., Laher, R. R., Shupe, D. L., Graham, M., Kasliwal, M., and Walters, R.

Abstract

In the new era of time-domain surveys, Type Ia supernovae are being caught sooner after explosion, which has exposed significant variation in their early light curves. Two driving factors for early-time evolution are the distribution of 56Ni in the ejecta and the presence of flux excesses of various causes. We perform an analysis of the largest young SN Ia sample to date. We compare 115 SN Ia light curves from the Zwicky Transient Facility to the TURTLS model grid containing light curves of Chandrasekhar mass explosions with a range of 56Ni masses, 56Ni distributions, and explosion energies. We find that the majority of our observed light curves are well reproduced by Chandrasekhar mass explosion models with a preference for highly extended 56Ni distributions. We identify six SNe Ia with an early-time flux excess in our gr-band data (four ‘blue’ and two ‘red’ flux excesses). We find an intrinsic rate of 18 ± 11 per cent of early flux excesses in SNe Ia at z < 0.07, based on three detected flux excesses out of 30 (10 per cent) observed SNe Ia with a simulated efficiency of 57 per cent. This is comparable to rates of flux excesses in the literature but also accounts for detection efficiencies. Two of these events are mostly consistent with circumstellar material interaction, while the other four have longer lifetimes in agreement with companion interaction and 56Ni-clump models. We find a higher frequency of flux excesses in 91T/99aa-like events (44 ± 13 per cent).

Published
2022
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3. A WC/WO star exploding within an expanding carbon-oxygen-neon nebula

Author

Gal-Yam, A., Bruch, R., Schulze, Steve, Yang, Y., Perley, D. A., Irani, I., Sollerman, Jesper, Kool, Erik C., Soumagnac, M. T., Yaron, O., Strotjohann, N. L., Zimmerman, E., Barbarino, Cristina, Kulkarni, S. R., Kasliwal, M. M., De, K., Yao, Y., Fremling, C., Yan, L., Ofek, E. O., Fransson, Claes, Filippenko, A. V., Zheng, W., Brink, T. G., Copperwheat, C. M., Foley, R. J., Brown, J., Siebert, M., Leloudas, G., Cabrera-Lavers, A. L., Garcia-Alvarez, D., Marante-Barreto, A., Frederick, S., Hung, T., Wheeler, J. C., Vinkó, J., Thomas, B. P., Graham, M. J., Duev, D. A., Drake, A. J., Dekany, R., Bellm, E. C., Rusholme, B., Shupe, D. L., Andreoni, I., Sharma, Y., Riddle, R., van Roestel, J., Knezevic, N., Gal-Yam, A., Bruch, R., Schulze, Steve, Yang, Y., Perley, D. A., Irani, I., Sollerman, Jesper, Kool, Erik C., Soumagnac, M. T., Yaron, O., Strotjohann, N. L., Zimmerman, E., Barbarino, Cristina, Kulkarni, S. R., Kasliwal, M. M., De, K., Yao, Y., Fremling, C., Yan, L., Ofek, E. O., Fransson, Claes, Filippenko, A. V., Zheng, W., Brink, T. G., Copperwheat, C. M., Foley, R. J., Brown, J., Siebert, M., Leloudas, G., Cabrera-Lavers, A. L., Garcia-Alvarez, D., Marante-Barreto, A., Frederick, S., Hung, T., Wheeler, J. C., Vinkó, J., Thomas, B. P., Graham, M. J., Duev, D. A., Drake, A. J., Dekany, R., Bellm, E. C., Rusholme, B., Shupe, D. L., Andreoni, I., Sharma, Y., Riddle, R., van Roestel, J., and Knezevic, N.

Abstract

The final fate of massive stars, and the nature of the compact remnants they leave behind (black holes and neutron stars), are open questions in astrophysics. Many massive stars are stripped of their outer hydrogen envelopes as they evolve. Such Wolf-Rayet stars(1) emit strong and rapidly expanding winds with speeds greater than 1,000 kilometres per second. A fraction of this population is also helium-depleted, with spectra dominated by highly ionized emission lines of carbon and oxygen (types WC/WO). Evidence indicates that the most commonly observed supernova explosions that lack hydrogen and helium (types Ib/Ic) cannot result from massive WC/WO stars(2,3), leading some to suggest that most such stars collapse directly into black holes without a visible supernova explosion(4). Here we report observations of SN 2019hgp, beginning about a day after the explosion. Its short rise time and rapid decline place it among an emerging population of rapidly evolving transients(5-8). Spectroscopy reveals a rich set of emission lines indicating that the explosion occurred within a nebula composed of carbon, oxygen and neon. Narrow absorption features show that this material is expanding at high velocities (greater than 1,500 kilometres per second), requiring a compact progenitor. Our observations are consistent with an explosion of a massive WC/WO star, and suggest that massive Wolf-Rayet stars may be the progenitors of some rapidly evolving transients.

Published
2022
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4. A WC/WO star exploding within an expanding carbon–oxygen–neon nebula

Author

Gal-Yam, A., Bruch, R., Schulze, S., Yang, Y., Perley, D. A., Irani, I., Sollerman, J., Kool, E. C., Soumagnac, M. T., Yaron, O., Strotjohann, N. L., Zimmerman, E., Barbarino, C., Kulkarni, S. R., Kasliwal, M. M., De, K., Yao, Y., Fremling, C., Yan, L., Ofek, E. O., Fransson, C., Filippenko, A. V., Zheng, W., Brink, T. G., Copperwheat, C. M., Foley, R. J., Brown, J., Siebert, M., Leloudas, G., Cabrera-Lavers, A. L., Garcia-Alvarez, D., Marante-Barreto, A., Frederick, S., Hung, T., Wheeler, J. C., Vinkó, J., Thomas, B. P., Graham, M. J., Duev, D. A., Drake, A. J., Dekany, R., Bellm, E. C., Rusholme, B., Shupe, D. L., Andreoni, I., Sharma, Y., Riddle, R., van Roestel, J., Knezevic, N., Gal-Yam, A., Bruch, R., Schulze, S., Yang, Y., Perley, D. A., Irani, I., Sollerman, J., Kool, E. C., Soumagnac, M. T., Yaron, O., Strotjohann, N. L., Zimmerman, E., Barbarino, C., Kulkarni, S. R., Kasliwal, M. M., De, K., Yao, Y., Fremling, C., Yan, L., Ofek, E. O., Fransson, C., Filippenko, A. V., Zheng, W., Brink, T. G., Copperwheat, C. M., Foley, R. J., Brown, J., Siebert, M., Leloudas, G., Cabrera-Lavers, A. L., Garcia-Alvarez, D., Marante-Barreto, A., Frederick, S., Hung, T., Wheeler, J. C., Vinkó, J., Thomas, B. P., Graham, M. J., Duev, D. A., Drake, A. J., Dekany, R., Bellm, E. C., Rusholme, B., Shupe, D. L., Andreoni, I., Sharma, Y., Riddle, R., van Roestel, J., and Knezevic, N.

Abstract

The final fate of massive stars, and the nature of the compact remnants they leave behind (black holes and neutron stars), are open questions in astrophysics. Many massive stars are stripped of their outer hydrogen envelopes as they evolve. Such Wolf–Rayet stars1 emit strong and rapidly expanding winds with speeds greater than 1,000 kilometres per second. A fraction of this population is also helium-depleted, with spectra dominated by highly ionized emission lines of carbon and oxygen (types WC/WO). Evidence indicates that the most commonly observed supernova explosions that lack hydrogen and helium (types Ib/Ic) cannot result from massive WC/WO stars2,3, leading some to suggest that most such stars collapse directly into black holes without a visible supernova explosion4. Here we report observations of SN 2019hgp, beginning about a day after the explosion. Its short rise time and rapid decline place it among an emerging population of rapidly evolving transients5–8. Spectroscopy reveals a rich set of emission lines indicating that the explosion occurred within a nebula composed of carbon, oxygen and neon. Narrow absorption features show that this material is expanding at high velocities (greater than 1,500 kilometres per second), requiring a compact progenitor. Our observations are consistent with an explosion of a massive WC/WO star, and suggest that massive Wolf–Rayet stars may be the progenitors of some rapidly evolving transients.

Published
2022

5. A WC/WO star exploding within an expanding carbon-oxygen-neon nebula

Author

Gal-Yam, A., Bruch, R., Schulze, S., Yang, Y., Perley, D. A., Irani, I., Sollerman, J., Kool, E. C., Soumagnac, M. T., Yaron, O., Strotjohann, N. L., Zimmerman, E., Barbarino, C., Kulkarni, S. R., Kasliwal, M. M., De, K., Yao, Y., Fremling, C., Yan, L., Ofek, E. O., Fransson, C., Filippenko, A. V., Zheng, W., Brink, T. G., Copperwheat, C. M., Foley, R. J., Brown, J., Siebert, M., Leloudas, G., Cabrera-Lavers, A. L., Garcia-Alvarez, D., Marante-Barreto, A., Frederick, S., Hung, T., Wheeler, J. C., Vinko, J., Thomas, B. P., Graham, M. J., Duev, D. A., Drake, A. J., Dekany, R., Bellm, E. C., Rusholme, B., Shupe, D. L., Andreoni, I., Sharma, Y., Riddle, R., van Roestel, J., Knezevic, N., Gal-Yam, A., Bruch, R., Schulze, S., Yang, Y., Perley, D. A., Irani, I., Sollerman, J., Kool, E. C., Soumagnac, M. T., Yaron, O., Strotjohann, N. L., Zimmerman, E., Barbarino, C., Kulkarni, S. R., Kasliwal, M. M., De, K., Yao, Y., Fremling, C., Yan, L., Ofek, E. O., Fransson, C., Filippenko, A. V., Zheng, W., Brink, T. G., Copperwheat, C. M., Foley, R. J., Brown, J., Siebert, M., Leloudas, G., Cabrera-Lavers, A. L., Garcia-Alvarez, D., Marante-Barreto, A., Frederick, S., Hung, T., Wheeler, J. C., Vinko, J., Thomas, B. P., Graham, M. J., Duev, D. A., Drake, A. J., Dekany, R., Bellm, E. C., Rusholme, B., Shupe, D. L., Andreoni, I., Sharma, Y., Riddle, R., van Roestel, J., and Knezevic, N.

Abstract

The final explosive fate of massive stars, and the nature of the compact remnants they leave behind (black holes and neutron stars), are major open questions in astrophysics. Many massive stars are stripped of their outer hydrogen envelopes as they evolve. Such Wolf-Rayet (W-R) stars emit strong and rapidly expanding (v_wind>1000 km/s) winds indicating a high escape velocity from the stellar surface. A fraction of this population is also helium depleted, with spectra dominated by highly-ionized emission lines of carbon and oxygen (Types WC/WO). Evidence indicates that the most commonly-observed supernova (SN) explosions that lack hydrogen and helium (Types Ib/Ic) cannot result from massive WC/WO stars, leading some to suggest that most such stars collapse directly into black holes without a visible supernova explosions. Here, we present observations of supernova SN 2019hgp, discovered about a day after explosion. The short rise time and rapid decline place it among an emerging population of rapidly-evolving transients (RETs). Spectroscopy reveals a rich set of emission lines indicating that the explosion occurred within a nebula composed of carbon, oxygen, and neon. Narrow absorption features show that this material is expanding at relatively high velocities (>1500 km/s) requiring a compact progenitor. Our observations are consistent with an explosion of a massive WC/WO star, and suggest that massive W-R stars may be the progenitors of some rapidly evolving transients., Comment: Unedited author version, Nature in press

Published
2021
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6. A WC/WO star exploding within an expanding carbon-oxygen-neon nebula

Author

Gal-Yam, A., Bruch, R., Schulze, S., Yang, Y., Perley, D. A., Irani, I., Sollerman, J., Kool, E. C., Soumagnac, M. T., Yaron, O., Strotjohann, N. L., Zimmerman, E., Barbarino, C., Kulkarni, S. R., Kasliwal, M. M., De, K., Yao, Y., Fremling, C., Yan, L., Ofek, E. O., Fransson, C., Filippenko, A. V., Zheng, W., Brink, T. G., Copperwheat, C. M., Foley, R. J., Brown, J., Siebert, M., Leloudas, G., Cabrera-Lavers, A. L., Garcia-Alvarez, D., Marante-Barreto, A., Frederick, S., Hung, T., Wheeler, J. C., Vinko, J., Thomas, B. P., Graham, M. J., Duev, D. A., Drake, A. J., Dekany, R., Bellm, E. C., Rusholme, B., Shupe, D. L., Andreoni, I., Sharma, Y., Riddle, R., van Roestel, J., Knezevic, N., Gal-Yam, A., Bruch, R., Schulze, S., Yang, Y., Perley, D. A., Irani, I., Sollerman, J., Kool, E. C., Soumagnac, M. T., Yaron, O., Strotjohann, N. L., Zimmerman, E., Barbarino, C., Kulkarni, S. R., Kasliwal, M. M., De, K., Yao, Y., Fremling, C., Yan, L., Ofek, E. O., Fransson, C., Filippenko, A. V., Zheng, W., Brink, T. G., Copperwheat, C. M., Foley, R. J., Brown, J., Siebert, M., Leloudas, G., Cabrera-Lavers, A. L., Garcia-Alvarez, D., Marante-Barreto, A., Frederick, S., Hung, T., Wheeler, J. C., Vinko, J., Thomas, B. P., Graham, M. J., Duev, D. A., Drake, A. J., Dekany, R., Bellm, E. C., Rusholme, B., Shupe, D. L., Andreoni, I., Sharma, Y., Riddle, R., van Roestel, J., and Knezevic, N.

Abstract

The final explosive fate of massive stars, and the nature of the compact remnants they leave behind (black holes and neutron stars), are major open questions in astrophysics. Many massive stars are stripped of their outer hydrogen envelopes as they evolve. Such Wolf-Rayet (W-R) stars emit strong and rapidly expanding (v_wind>1000 km/s) winds indicating a high escape velocity from the stellar surface. A fraction of this population is also helium depleted, with spectra dominated by highly-ionized emission lines of carbon and oxygen (Types WC/WO). Evidence indicates that the most commonly-observed supernova (SN) explosions that lack hydrogen and helium (Types Ib/Ic) cannot result from massive WC/WO stars, leading some to suggest that most such stars collapse directly into black holes without a visible supernova explosions. Here, we present observations of supernova SN 2019hgp, discovered about a day after explosion. The short rise time and rapid decline place it among an emerging population of rapidly-evolving transients (RETs). Spectroscopy reveals a rich set of emission lines indicating that the explosion occurred within a nebula composed of carbon, oxygen, and neon. Narrow absorption features show that this material is expanding at relatively high velocities (>1500 km/s) requiring a compact progenitor. Our observations are consistent with an explosion of a massive WC/WO star, and suggest that massive W-R stars may be the progenitors of some rapidly evolving transients., Comment: Unedited author version, Nature in press

Published
2021
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7. ZTF Early Observations of Type Ia Supernovae. III. Early-time Colors As a Test for Explosion Models and Multiple Populations

Author

Bulla, Mattia, Miller, A. A., Yao, Y., Dessart, L., Dhawan, S., Papadogiannakis, S., Biswas, R., Goobar, A., Kulkarni, S. R., Nordin, J., Nugent, P., Polin, A., Sollerman, J., Bellm, E. C., Coughlin, M. W., Dekany, R., Golkhou, V. Z., Graham, M. J., Kasliwal, M. M., Kupfer, T., Laher, R. R., Masci, F. J., Porter, M., Rusholme, B., Shupe, D. L., Bulla, Mattia, Miller, A. A., Yao, Y., Dessart, L., Dhawan, S., Papadogiannakis, S., Biswas, R., Goobar, A., Kulkarni, S. R., Nordin, J., Nugent, P., Polin, A., Sollerman, J., Bellm, E. C., Coughlin, M. W., Dekany, R., Golkhou, V. Z., Graham, M. J., Kasliwal, M. M., Kupfer, T., Laher, R. R., Masci, F. J., Porter, M., Rusholme, B., and Shupe, D. L.

Abstract

Colors of Type Ia supernovae (SNe Ia) in the first few days after explosion provide a potential discriminant between different models. In this paper, we present g-r colors of 65 SNe Ia discovered within 5 days from first light by the Zwicky Transient Facility in 2018, a sample that is about three times larger than that in the literature. We find that g-r colors are intrinsically rather homogeneous at early phases, with about half of the dispersion attributable to photometric uncertainties (σnoise ∼ σ int ∼ 0.18 mag). Colors are nearly constant starting from 6 days after first light (g-r ∼-0.15 mag), while the time evolution at earlier epochs is characterized by a continuous range of slopes, from events rapidly transitioning from redder to bluer colors (slope of ∼-0.25 mag day-1) to events with a flatter evolution. The continuum in the slope distribution is in good agreement both with models requiring some amount of 56Ni mixed in the outermost regions of the ejecta and with "double-detonation"models having thin helium layers MHe=0.01 M⊙) and varying carbon-oxygen core masses. At the same time, six events show evidence for a distinctive "red bump"signature predicted by double-detonation models with larger helium masses. We finally identify a significant correlation between the early-time g-r slopes and supernova brightness, with brighter events associated to flatter color evolution (p-value = 0.006). The distribution of slopes, however, is consistent with being drawn from a single population, with no evidence for two components as claimed in the literature based on B-V colors., QC 20210223

Published
2020
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8. Optical follow-up of the neutron star–black hole mergers S200105ae and S200115j

Author

Anand, S., Coughlin, M. W., Kasliwal, M. M., Bulla, Mattia, Ahumada, T., Sagués Carracedo, A., Almualla, M., Andreoni, I., Stein, R., Foucart, F., Singer, L. P., Sollerman, J., Bellm, E. C., Bolin, B., Caballero-García, M. D., Castro-Tirado, A. J., Cenko, S. B., De, K., Dekany, R. G., Duev, D. A., Feeney, M., Fremling, C., Goldstein, D. A., Golkhou, V. Z., Graham, M. J., Guessoum, N., Hankins, M. J., Hu, Y., Kong, A. K. H., Kool, E. C., Kulkarni, S. R., Kumar, H., Laher, R. R., Masci, F. J., Mróz, P., Nissanke, S., Porter, M., Reusch, S., Riddle, R., Rosnet, P., Rusholme, B., Serabyn, E., Sánchez-Ramírez, R., Rigault, M., Shupe, D. L., Smith, R., Soumagnac, M. T., Walters, R., Valeev, Azamat F., Anand, S., Coughlin, M. W., Kasliwal, M. M., Bulla, Mattia, Ahumada, T., Sagués Carracedo, A., Almualla, M., Andreoni, I., Stein, R., Foucart, F., Singer, L. P., Sollerman, J., Bellm, E. C., Bolin, B., Caballero-García, M. D., Castro-Tirado, A. J., Cenko, S. B., De, K., Dekany, R. G., Duev, D. A., Feeney, M., Fremling, C., Goldstein, D. A., Golkhou, V. Z., Graham, M. J., Guessoum, N., Hankins, M. J., Hu, Y., Kong, A. K. H., Kool, E. C., Kulkarni, S. R., Kumar, H., Laher, R. R., Masci, F. J., Mróz, P., Nissanke, S., Porter, M., Reusch, S., Riddle, R., Rosnet, P., Rusholme, B., Serabyn, E., Sánchez-Ramírez, R., Rigault, M., Shupe, D. L., Smith, R., Soumagnac, M. T., Walters, R., and Valeev, Azamat F.

Abstract

LIGO and Virgo’s third observing run revealed the first neutron star–black hole (NSBH) merger candidates in gravitational waves. These events are predicted to synthesize r-process elements1,2 creating optical/near-infrared ‘kilonova’ emission. The joint gravitational wave and electromagnetic detection of an NSBH merger could be used to constrain the equation of state of dense nuclear matter3, and independently measure the local expansion rate of the Universe4. Here, we present the optical follow-up and analysis of two of the only three high-significance NSBH merger candidates detected to date, S200105ae and S200115j, with the Zwicky Transient Facility5. The Zwicky Transient Facility observed ~48% of S200105ae and ~22% of S200115j’s localization probabilities, with observations sensitive to kilonovae brighter than −17.5 mag fading at 0.5 mag d−1 in the g- and r-bands; extensive searches and systematic follow-up of candidates did not yield a viable counterpart. We present state-of-the-art kilonova models tailored to NSBH systems that place constraints on the ejecta properties of these NSBH mergers. We show that with observed depths of apparent magnitude ~22 mag, attainable in metre-class, wide-field-of-view survey instruments, strong constraints on ejecta mass are possible, with the potential to rule out low mass ratios, high black hole spins and large neutron star radii., QC 20201117

Published
2020
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9. ZTF Early Observations of Type Ia Supernovae. II. First Light, the Initial Rise, and Time to Reach Maximum Brightness

Author

Miller, A. A., Yao, Y., Bulla, M., Pankow, C., Bellm, E. C., Cenko, S. B., Dekany, R., Fremling, C., Graham, M. J., Kupfer, T., Laher, R. R., Mahabal, A. A., Masci, F. J., Nugent, P. E., Riddle, R., Rusholme, B., Smith, R. M., Shupe, D. L., Roestel, J. van, Kulkarni, S. R., Miller, A. A., Yao, Y., Bulla, M., Pankow, C., Bellm, E. C., Cenko, S. B., Dekany, R., Fremling, C., Graham, M. J., Kupfer, T., Laher, R. R., Mahabal, A. A., Masci, F. J., Nugent, P. E., Riddle, R., Rusholme, B., Smith, R. M., Shupe, D. L., Roestel, J. van, and Kulkarni, S. R.

Abstract

While it is clear that Type Ia supernovae (SNe) are the result of thermonuclear explosions in C/O white dwarfs (WDs), a great deal remains uncertain about the binary companion that facilitates the explosive disruption of the WD. Here, we present a comprehensive analysis of a large, unique data set of 127 SNe Ia with exquisite coverage by the Zwicky Transient Facility (ZTF). High-cadence (six observations per night) ZTF observations allow us to measure the SN rise time and examine its initial evolution. We develop a Bayesian framework to model the early rise as a power law in time, which enables the inclusion of priors in our model. For a volume-limited subset of normal SNe Ia, we find that the mean power-law index is consistent with 2 in the r(ZTF)-band (alpha(r) = 2.01 +/- 0.02), as expected in the expanding fireball model. There are, however, individual SNe that are clearly inconsistent with alpha(r) = 2. We estimate a mean rise time of 18.9 days (with a range extending from similar to 15 to 22 days), though this is subject to the adopted prior. We identify an important, previously unknown, bias whereby the rise times for higherredshift SNe within a flux-limited survey are systematically underestimated. This effect can be partially alleviated if the power-law index is fixed to alpha = 2, in which case we estimate a mean rise time of 21.7 days (with a range from similar to 18 to 23 days). The sample includes a handful of rare and peculiar SNe Ia. Finally, we conclude with a discussion of lessons learned from the ZTF sample that can eventually be applied to observations from the Vera C..Rubin Observatory., QC 20220922Nordita SU

Published
2020
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10. The Zwicky Transient Facility Bright Transient Survey. I. Spectroscopic Classification and the Redshift Completeness of Local Galaxy Catalogs

Author

Fremling, C., Miller, A. A., Sharma, Y., Dugas, A., Perley, D. A., Taggart, K., Sollerman, Jesper, Goobar, Ariel, Graham, M. L., Neill, J. D., Nordin, J., Rigault, M., Walters, R., Andreoni, I., Bagdasaryan, A., Belicki, J., Cannella, C., Bellm, E. C., Cenko, S. B., De, K., Dekany, R., Frederick, S., Golkhou, V. Z., Graham, M. J., Helou, G., Ho, A. Y. Q., Kasliwal, M. M., Kupfer, T., Laher, R. R., Mahabal, A., Masci, F. J., Riddle, R., Rusholme, B., Schulze, S., Shupe, D. L., Smith, R. M., van Velzen, S., Yan, Lin, Yao, Y., Zhuang, Z., Kulkarni, S. R., Fremling, C., Miller, A. A., Sharma, Y., Dugas, A., Perley, D. A., Taggart, K., Sollerman, Jesper, Goobar, Ariel, Graham, M. L., Neill, J. D., Nordin, J., Rigault, M., Walters, R., Andreoni, I., Bagdasaryan, A., Belicki, J., Cannella, C., Bellm, E. C., Cenko, S. B., De, K., Dekany, R., Frederick, S., Golkhou, V. Z., Graham, M. J., Helou, G., Ho, A. Y. Q., Kasliwal, M. M., Kupfer, T., Laher, R. R., Mahabal, A., Masci, F. J., Riddle, R., Rusholme, B., Schulze, S., Shupe, D. L., Smith, R. M., van Velzen, S., Yan, Lin, Yao, Y., Zhuang, Z., and Kulkarni, S. R.

Abstract

The Zwicky Transient Facility (ZTF) is performing a three-day cadence survey of the visible northern sky (similar to 3 pi) with newly found transient candidates announced via public alerts. The ZTF Bright Transient Survey (BTS) is a large spectroscopic campaign to complement the photometric survey. BTS endeavors to spectroscopically classify all extragalactic transients with m(peak) <= 18.5 mag in either the g(ZTF) or r(ZTF) filters, and publicly announce said classifications. BTS discoveries are predominantly supernovae (SNe), making this the largest flux-limited SN survey to date. Here we present a catalog of 761 SNe, classified during the first nine months of ZTF (2018 April 1-2018 December 31). We report BTS SN redshifts from SN template matching and spectroscopic host-galaxy redshifts when available. We analyze the redshift completeness of local galaxy catalogs, the redshift completeness fraction (RCF; the ratio of SN host galaxies with known spectroscopic redshift prior to SN discovery to the total number of SN hosts). Of the 512 host galaxies with SNe Ia, 227 had previously known spectroscopic redshifts, yielding an RCF estimate of 44% 4%. The RCF decreases with increasing distance and decreasing galaxy luminosity (for z < 0.05, or similar to 200 Mpc, RCF 0.6). Prospects for dramatically increasing the RCF are limited to new multifiber spectroscopic instruments or wide-field narrowband surveys. Existing galaxy redshift catalogs are only similar to 50% complete at r 16.9 mag. Pushing this limit several magnitudes deeper will pay huge dividends when searching for electromagnetic counterparts to gravitational wave events or sources of ultra-high-energy cosmic rays or neutrinos.

Published
2020
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11. Helium-rich Superluminous Supernovae from the Zwicky Transient Facility

Author

Yan, Lin, Perley, D. A., Schulze, S., Lunnan, Ragnhild, Sollerman, Jesper, De, K., Chen, Z. H., Fremling, C., Gal-Yam, A., Taggart, K., Chen, Ting-Wan, Andreoni, I., Bellm, E. C., Cunningham, V., Dekany, R., Duev, D. A., Fransson, Claes, Laher, R. R., Hankins, M., Ho, A. Y. Q., Jencson, J. E., Kaye, S., Kulkarni, S. R., Kasliwal, M. M., Golkhou, V. Z., Graham, M., Masci, F. J., Miller, A. A., Neill, J. D., Ofek, E., Porter, M., Mroz, P., Reiley, D., Riddle, R., Rigault, M., Rusholme, B., Shupe, D. L., Soumagnac, M. T., Smith, R., Tartaglia, Leonardo, Yao, Y., Yaron, O., Yan, Lin, Perley, D. A., Schulze, S., Lunnan, Ragnhild, Sollerman, Jesper, De, K., Chen, Z. H., Fremling, C., Gal-Yam, A., Taggart, K., Chen, Ting-Wan, Andreoni, I., Bellm, E. C., Cunningham, V., Dekany, R., Duev, D. A., Fransson, Claes, Laher, R. R., Hankins, M., Ho, A. Y. Q., Jencson, J. E., Kaye, S., Kulkarni, S. R., Kasliwal, M. M., Golkhou, V. Z., Graham, M., Masci, F. J., Miller, A. A., Neill, J. D., Ofek, E., Porter, M., Mroz, P., Reiley, D., Riddle, R., Rigault, M., Rusholme, B., Shupe, D. L., Soumagnac, M. T., Smith, R., Tartaglia, Leonardo, Yao, Y., and Yaron, O.

Abstract

Helium is expected to be present in the massive ejecta of some hydrogen-poor superluminous supernovae (SLSN-I). However, until now only one event has been identified with He features in its photospheric spectra (PTF10hgi). We present the discovery of a new He-rich SLSN-I, ZTF19aawfbtg (SN2019hge), atz = 0.0866. This event has more than 10 optical spectra at phases from -41 to +103 days relative to the peak, most of which match well with that of PTF10hgi. Confirmation comes from a near-IR spectrum taken at +34 days, revealing Heifeatures with P-Cygni profiles at 1.083 and 2.058 mu m. Using the optical spectra of PTF10hgi and SN2019hge as templates, we examined 70 other SLSNe-I discovered by Zwicky Transient Facility in the first two years of operation and found five additional SLSNe-I with distinct He-features. The excitation of Heiatoms in normal core-collapse supernovae requires nonthermal radiation, as proposed by previous studies. These He-rich events cannot be explained by the traditional(56)Ni mixing model because of their blue spectra, high peak luminosities, and long rise timescales. Magnetar models offer a possible solution since pulsar winds naturally generate high-energy particles, potential sources of nonthermal excitation. An alternative model is the interaction between the ejecta and dense H-poor circumstellar material, which may be supported by observed undulations in the light curves. These six SLSNe-Ib have relatively low-peak luminosities (rest frameM(g) = -20.06 0.16).

Published
2020
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12. Four (Super)luminous Supernovae from the First Months of the ZTF Survey

Author

Lunnan, Ragnhild, Yan, Lin, Perley, D. A., Schulze, S., Taggart, K., Gal-Yam, A., Fremling, C., Soumagnac, M. T., Ofek, E., Adams, S. M., Barbarino, Cristina, Bellm, E. C., De, K., Fransson, Claes, Frederick, S., Golkhou, V. Z., Graham, M. J., Hallakoun, N., Ho, A. Y. Q., Kasliwal, M. M., Kaspi, S., Kulkarni, S. R., Laher, R. R., Masci, F. J., Nunez, F. Pozo, Rusholme, B., Quimby, R. M., Shupe, D. L., Sollerman, Jesper, Taddia, Francesco, van Roestel, J., Yang, Y., Yao, Yuhan, Lunnan, Ragnhild, Yan, Lin, Perley, D. A., Schulze, S., Taggart, K., Gal-Yam, A., Fremling, C., Soumagnac, M. T., Ofek, E., Adams, S. M., Barbarino, Cristina, Bellm, E. C., De, K., Fransson, Claes, Frederick, S., Golkhou, V. Z., Graham, M. J., Hallakoun, N., Ho, A. Y. Q., Kasliwal, M. M., Kaspi, S., Kulkarni, S. R., Laher, R. R., Masci, F. J., Nunez, F. Pozo, Rusholme, B., Quimby, R. M., Shupe, D. L., Sollerman, Jesper, Taddia, Francesco, van Roestel, J., Yang, Y., and Yao, Yuhan

Abstract

We present photometry and spectroscopy of four hydrogen-poor luminous supernovae discovered during the 2-month long science commissioning and early operations of the Zwicky Transient Facility (ZTF) survey. Three of these objects, SN 2018bym (ZTF18aapgrxo), SN 2018avk (ZTF18aaisyyp), and SN 2018bgv (ZTF18aavrmcg), resemble typical SLSN-I spectroscopically, while SN 2018don (ZTF18aajqcue) may be an object similar to SN 2007bi experiencing considerable host galaxy reddening, or an intrinsically long-lived, luminous, and red SN Ic. We analyze the light curves, spectra, and host galaxy properties of these four objects and put them in context of the population of SLSN-I. SN 2018bgv stands out as the fastest-rising SLSN-I observed to date, with a rest-frame g-band rise time of just 10 days from explosion to peak—if it is powered by magnetar spin-down, the implied ejecta mass is only 1 M ⊙. SN 2018don also displays unusual properties—in addition to its red colors and comparatively massive host galaxy, the light curve undergoes some of the strongest light-curve undulations postpeak seen in an SLSN-I, which we speculate may be due to interaction with circumstellar material. We discuss the promises and challenges of finding SLSNe in large-scale surveys like ZTF given the observed diversity in the population.

Published
2020
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13. The Koala: A Fast Blue Optical Transient with Luminous Radio Emission from a Starburst Dwarf Galaxy at $z=0.27$

Author

Ho, Anna Y. Q., Perley, D. A., Kulkarni, S. R., Dong, D. Z. J., De, K., Chandra, P., Andreoni, I., Bellm, E. C., Burdge, K. B., Coughlin, M., Dekany, R., Feeney, M., Frederiks, D. D., Fremling, C., Golkhou, V. Z., Graham, M., Hale, D., Helou, G., Horesh, A., Laher, R. R., Masci, F., Miller, A. A., Porter, M., Ridnaia, A., Rusholme, B., Shupe, D. L., Soumagnac, M. T., Svinkin, D. S., Ho, Anna Y. Q., Perley, D. A., Kulkarni, S. R., Dong, D. Z. J., De, K., Chandra, P., Andreoni, I., Bellm, E. C., Burdge, K. B., Coughlin, M., Dekany, R., Feeney, M., Frederiks, D. D., Fremling, C., Golkhou, V. Z., Graham, M., Hale, D., Helou, G., Horesh, A., Laher, R. R., Masci, F., Miller, A. A., Porter, M., Ridnaia, A., Rusholme, B., Shupe, D. L., Soumagnac, M. T., and Svinkin, D. S.

Abstract

We present ZTF18abvkwla (the "Koala"), a fast blue optical transient discovered in the Zwicky Transient Facility (ZTF) One-Day Cadence (1DC) Survey. ZTF18abvkwla has a number of features in common with the groundbreaking transient AT2018cow: blue colors at peak ($g-r\approx-0.5$ mag), a short rise time from half-max of under two days, a decay time to half-max of only three days, a high optical luminosity ($M_{g,\mathrm{peak}}\approx-20.6$mag), a hot ($\gtrsim 40,000$K) featureless spectrum at peak light, and a luminous radio counterpart. At late times ($\Delta t>80$d) the radio luminosity of ZTF18abvkwla ($\nu L_\nu \gtrsim 10^{40}$erg/s at 10 GHz, observer-frame) is most similar to that of long-duration gamma-ray bursts (GRBs). The host galaxy is a dwarf starburst galaxy ($M\approx5\times10^{8}M_\odot$, $\mathrm{SFR}\approx7 M_\odot$/yr) that is moderately metal-enriched ($\log\mathrm{[O/H]} \approx 8.5$), similar to the hosts of GRBs and superluminous supernovae. As in AT2018cow, the radio and optical emission in ZTF18abvkwla likely arise from two separate components: the radio from fast-moving ejecta ($\Gamma \beta c >0.38c$) and the optical from shock-interaction with confined dense material ($<0.07M_\odot$ in $\sim 10^{15}$cm). Compiling transients in the literature with $t_\mathrm{rise} <5$d and $M_\mathrm{peak}<-20$mag, we find that a significant number are engine-powered, and suggest that the high peak optical luminosity is directly related to the presence of this engine. From 18 months of the 1DC survey, we find that transients in this rise-luminosity phase space are at least two to three orders of magnitude less common than CC SNe. Finally, we discuss strategies for identifying such events with future facilities like the Large Synoptic Survey Telescope, and prospects for detecting accompanying X-ray and radio emission., Comment: 27 pages, 11 figures. Resubmitted to ApJ on 13 April following comments by referee. Comments welcome!

Published
2020
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14. The Spectacular Ultraviolet Flash From the Peculiar Type Ia Supernova 2019yvq

Author

Miller, A. A., Magee, M. R., Polin, A., Maguire, K., Zimmerman, E., Yao, Y., Sollerman, J., Schulze, S., Perley, D. A., Kromer, M., Bulla, M., Andreoni, I., Bellm, E. C., De, K., Dekany, R., Delacroix, A., Dhawan, S., Fremling, C., Gal-Yam, A., Goldstein, D. A., Golkhou, V. Z., Goobar, A., Graham, M. J., Irani, I., Kasliwal, M. M., Kaye, S., Kim, Y. -L., Laher, R. R., Mahabal, A. A., Masci, F. J., Nugent, P. E., Ofek, E., Phinney, E. S., Prentice, S. J., Riddle, R., Rigault, M., Rusholme, B., Schweyer, T., Shupe, D. L., Soumagnac, M. T., Terreran, G., Walters, R., Yan, L., Zolkower, J., Kulkarni, S. R., Miller, A. A., Magee, M. R., Polin, A., Maguire, K., Zimmerman, E., Yao, Y., Sollerman, J., Schulze, S., Perley, D. A., Kromer, M., Bulla, M., Andreoni, I., Bellm, E. C., De, K., Dekany, R., Delacroix, A., Dhawan, S., Fremling, C., Gal-Yam, A., Goldstein, D. A., Golkhou, V. Z., Goobar, A., Graham, M. J., Irani, I., Kasliwal, M. M., Kaye, S., Kim, Y. -L., Laher, R. R., Mahabal, A. A., Masci, F. J., Nugent, P. E., Ofek, E., Phinney, E. S., Prentice, S. J., Riddle, R., Rigault, M., Rusholme, B., Schweyer, T., Shupe, D. L., Soumagnac, M. T., Terreran, G., Walters, R., Yan, L., Zolkower, J., and Kulkarni, S. R.

Abstract

Early observations of Type Ia supernovae (SNe$\,$Ia) provide essential clues for understanding the progenitor system that gave rise to the terminal thermonuclear explosion. We present exquisite observations of SN$\,$2019yvq, the second observed SN$\,$Ia, after iPTF$\,$14atg, to display an early flash of emission in the ultraviolet (UV) and optical. Our analysis finds that SN$\,$2019yvq was unusual, even when ignoring the initial flash, in that it was moderately underluminous for an SN$\,$Ia ($M_g \approx -18.5\,$mag at peak) yet featured very high absorption velocities ($v \approx 15,000\,\mathrm{km\,s}^{-1}$ for Si II $\lambda$6355 at peak). We find that many of the observational features of SN$\,$2019yvq, aside from the flash, can be explained if the explosive yield of radioactive $^{56}\mathrm{Ni}$ is relatively low (we measure $M_{^{56}\mathrm{Ni}} = 0.31 \pm 0.05\,M_\odot$) and it and other iron-group elements are concentrated in the innermost layers of the ejecta. To explain both the UV/optical flash and peak properties of SN$\,$2019yvq we consider four different models: interaction between the SN ejecta and a nondegenerate companion, extended clumps of $^{56}\mathrm{Ni}$ in the outer ejecta, a double-detonation explosion, and the violent merger of two white dwarfs. Each of these models has shortcomings when compared to the observations; it is clear additional tuning is required to better match SN$\,$2019yvq. In closing, we predict that the nebular spectra of SN$\,$2019yvq will feature either H or He emission, if the ejecta collided with a companion, strong [Ca II] emission, if it was a double detonation, or narrow [O I] emission, if it was due to a violent merger., Comment: 27 pages, 14 figures, accepted in ApJ

Published
2020
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15. SN2020bvc: a Broad-lined Type Ic Supernova with a Double-peaked Optical Light Curve and a Luminous X-ray and Radio Counterpart

Author

Ho, A. Y. Q., Kulkarni, S. R., Perley, D. A., Cenko, S. B., Corsi, A., Schulze, S., Lunnan, R., Sollerman, J., Gal-Yam, A., Anand, S., Barbarino, C., Bellm, E., Bruch, R., Burns, E., De, K., Dekany, R., Delacroix, A., Duev, D., Fremling, C., Goldstein, D., Golkhou, Z., Graham, M. J., Hale, D., Kasliwal, M. M., Kupfer, T., Laher, R., Martikainen, J., Masci, F. J., Neill, J. D., Rusholme, B., Shupe, D. L., Soumagnac, M. T., Strotjohann, N. L., Taggart, K., Tartaglia, L., Yan, L., Zolkower, J., Ho, A. Y. Q., Kulkarni, S. R., Perley, D. A., Cenko, S. B., Corsi, A., Schulze, S., Lunnan, R., Sollerman, J., Gal-Yam, A., Anand, S., Barbarino, C., Bellm, E., Bruch, R., Burns, E., De, K., Dekany, R., Delacroix, A., Duev, D., Fremling, C., Goldstein, D., Golkhou, Z., Graham, M. J., Hale, D., Kasliwal, M. M., Kupfer, T., Laher, R., Martikainen, J., Masci, F. J., Neill, J. D., Rusholme, B., Shupe, D. L., Soumagnac, M. T., Strotjohann, N. L., Taggart, K., Tartaglia, L., Yan, L., and Zolkower, J.

Abstract

We present optical, radio, and X-ray observations of SN2020bvc (=ASASSN20bs; ZTF20aalxlis), a nearby ($z=0.0252$; $d$=114 Mpc) broad-lined (BL) Type Ic supernova (SN). Our observations show that SN2020bvc shares several properties in common with the Ic-BL SN2006aj, which was associated with the low-luminosity gamma-ray burst (LLGRB) 060218. First, the 10 GHz radio light curve is on the faint end of LLGRB-SNe ($L_\mathrm{radio} \approx 10^{37}$erg/s): we model our VLA observations (spanning 13-43 d) as synchrotron emission from a mildly relativistic ($v \gtrsim 0.3c$) forward shock. Second, with Swift and Chandra we detect X-ray emission ($L_X \approx 10^{41}$erg/s) that is not naturally explained as inverse Compton emission or as part of the same synchrotron spectrum as the radio emission. Third, high-cadence ($6\times$/night) data from the Zwicky Transient Facility (ZTF) shows a double-peaked optical light curve, the first peak from shock-cooling emission from extended low-mass material (mass $M<10^{-2} M_\odot$ at radius $R>10^{12}$cm) and the second peak from the radioactive decay of Ni-56. SN2020bvc is the first confirmed double-peaked Ic-BL SN discovered without a GRB trigger, and shows X-ray and radio emission similar to LLGRB-SNe: this is consistent with models in which the same mechanism produces both the LLGRB and the shock-cooling emission. For four of the five other nearby ($z\lesssim0.05$) Ic-BL SNe with ZTF high-cadence data, we rule out a first peak like that seen in SN2006aj and SN2020bvc, i.e. that lasts $\approx 1$d and reaches a peak luminosity $M \approx -18$. X-ray and radio follow-up observations of future such events will establish whether double-peaked optical light curves are indeed predictive of LLGRB-like X-ray and radio emission., Comment: Accepted to ApJ. 39 pages, 17 figures. Comments welcome

Published
2020
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16. ZTF Early Observations of Type Ia Supernovae II: First Light, the Initial Rise, and Time to Reach Maximum Brightness

Author

Miller, A. A., Yao, Y., Bulla, M., Pankow, C., Bellm, E. C., Cenko, S. B., Dekany, R., Fremling, C., Graham, M. J., Kupfer, T., Laher, R. R., Mahabal, A. A., Masci, F. J., Nugent, P. E., Riddle, R., Rusholme, B., Smith, R. M., Shupe, D. L., van Roestel, J., Kulkarni, S. R., Miller, A. A., Yao, Y., Bulla, M., Pankow, C., Bellm, E. C., Cenko, S. B., Dekany, R., Fremling, C., Graham, M. J., Kupfer, T., Laher, R. R., Mahabal, A. A., Masci, F. J., Nugent, P. E., Riddle, R., Rusholme, B., Smith, R. M., Shupe, D. L., van Roestel, J., and Kulkarni, S. R.

Abstract

While it is clear that Type Ia supernovae (SNe) are the result of thermonuclear explosions in C/O white dwarfs (WDs), a great deal remains uncertain about the binary companion that facilitates the explosive disruption of the WD. Here, we present a comprehensive analysis of a large, unique data set of 127 SNe$\,$Ia with exquisite coverage by the Zwicky Transient Facility (ZTF). High-cadence (six observations per night) ZTF observations allow us to measure the SN rise time and examine its initial evolution. We develop a Bayesian framework to model the early rise as a power law in time, which enables the inclusion of priors in our model. For a volume-limited subset of normal SNe$\,$Ia, we find that the mean power-law index is consistent with 2 in the $r_\mathrm{ZTF}$-band ($\alpha_r = 2.01\pm0.02$), as expected in the expanding fireball model. There are, however, individual SNe that are clearly inconsistent with $\alpha_r=2$. We estimate a mean rise time of 18.9$\,$d (with a range extending from $\sim$15 to 22$\,$d), though this is subject to the adopted prior. We identify an important, previously unknown, bias whereby the rise times for higher-redshift SNe within a flux-limited survey are systematically underestimated. This effect can be partially alleviated if the power-law index is fixed to $\alpha=2$, in which case we estimate a mean rise time of 21.7$\,$d (with a range from $\sim$18 to 23$\,$d). The sample includes a handful of rare and peculiar SNe$\,$Ia. Finally, we conclude with a discussion of lessons learned from the ZTF sample that can eventually be applied to observations from the Vera C. Rubin Observatory., Comment: 31 pages, 17 figures; ApJ accepted

Published
2020
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17. The Spectacular Ultraviolet Flash From the Peculiar Type Ia Supernova 2019yvq

Author

Miller, A. A., Magee, M. R., Polin, A., Maguire, K., Zimmerman, E., Yao, Y., Sollerman, J., Schulze, S., Perley, D. A., Kromer, M., Bulla, M., Andreoni, I., Bellm, E. C., De, K., Dekany, R., Delacroix, A., Dhawan, S., Fremling, C., Gal-Yam, A., Goldstein, D. A., Golkhou, V. Z., Goobar, A., Graham, M. J., Irani, I., Kasliwal, M. M., Kaye, S., Kim, Y. -L., Laher, R. R., Mahabal, A. A., Masci, F. J., Nugent, P. E., Ofek, E., Phinney, E. S., Prentice, S. J., Riddle, R., Rigault, M., Rusholme, B., Schweyer, T., Shupe, D. L., Soumagnac, M. T., Terreran, G., Walters, R., Yan, L., Zolkower, J., Kulkarni, S. R., Miller, A. A., Magee, M. R., Polin, A., Maguire, K., Zimmerman, E., Yao, Y., Sollerman, J., Schulze, S., Perley, D. A., Kromer, M., Bulla, M., Andreoni, I., Bellm, E. C., De, K., Dekany, R., Delacroix, A., Dhawan, S., Fremling, C., Gal-Yam, A., Goldstein, D. A., Golkhou, V. Z., Goobar, A., Graham, M. J., Irani, I., Kasliwal, M. M., Kaye, S., Kim, Y. -L., Laher, R. R., Mahabal, A. A., Masci, F. J., Nugent, P. E., Ofek, E., Phinney, E. S., Prentice, S. J., Riddle, R., Rigault, M., Rusholme, B., Schweyer, T., Shupe, D. L., Soumagnac, M. T., Terreran, G., Walters, R., Yan, L., Zolkower, J., and Kulkarni, S. R.

Abstract

Early observations of Type Ia supernovae (SNe$\,$Ia) provide essential clues for understanding the progenitor system that gave rise to the terminal thermonuclear explosion. We present exquisite observations of SN$\,$2019yvq, the second observed SN$\,$Ia, after iPTF$\,$14atg, to display an early flash of emission in the ultraviolet (UV) and optical. Our analysis finds that SN$\,$2019yvq was unusual, even when ignoring the initial flash, in that it was moderately underluminous for an SN$\,$Ia ($M_g \approx -18.5\,$mag at peak) yet featured very high absorption velocities ($v \approx 15,000\,\mathrm{km\,s}^{-1}$ for Si II $\lambda$6355 at peak). We find that many of the observational features of SN$\,$2019yvq, aside from the flash, can be explained if the explosive yield of radioactive $^{56}\mathrm{Ni}$ is relatively low (we measure $M_{^{56}\mathrm{Ni}} = 0.31 \pm 0.05\,M_\odot$) and it and other iron-group elements are concentrated in the innermost layers of the ejecta. To explain both the UV/optical flash and peak properties of SN$\,$2019yvq we consider four different models: interaction between the SN ejecta and a nondegenerate companion, extended clumps of $^{56}\mathrm{Ni}$ in the outer ejecta, a double-detonation explosion, and the violent merger of two white dwarfs. Each of these models has shortcomings when compared to the observations; it is clear additional tuning is required to better match SN$\,$2019yvq. In closing, we predict that the nebular spectra of SN$\,$2019yvq will feature either H or He emission, if the ejecta collided with a companion, strong [Ca II] emission, if it was a double detonation, or narrow [O I] emission, if it was due to a violent merger., Comment: 27 pages, 14 figures, accepted in ApJ

Published
2020
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18. SN2020bvc: a Broad-lined Type Ic Supernova with a Double-peaked Optical Light Curve and a Luminous X-ray and Radio Counterpart

Author

Ho, A. Y. Q., Kulkarni, S. R., Perley, D. A., Cenko, S. B., Corsi, A., Schulze, S., Lunnan, R., Sollerman, J., Gal-Yam, A., Anand, S., Barbarino, C., Bellm, E., Bruch, R., Burns, E., De, K., Dekany, R., Delacroix, A., Duev, D., Fremling, C., Goldstein, D., Golkhou, Z., Graham, M. J., Hale, D., Kasliwal, M. M., Kupfer, T., Laher, R., Martikainen, J., Masci, F. J., Neill, J. D., Rusholme, B., Shupe, D. L., Soumagnac, M. T., Strotjohann, N. L., Taggart, K., Tartaglia, L., Yan, L., Zolkower, J., Ho, A. Y. Q., Kulkarni, S. R., Perley, D. A., Cenko, S. B., Corsi, A., Schulze, S., Lunnan, R., Sollerman, J., Gal-Yam, A., Anand, S., Barbarino, C., Bellm, E., Bruch, R., Burns, E., De, K., Dekany, R., Delacroix, A., Duev, D., Fremling, C., Goldstein, D., Golkhou, Z., Graham, M. J., Hale, D., Kasliwal, M. M., Kupfer, T., Laher, R., Martikainen, J., Masci, F. J., Neill, J. D., Rusholme, B., Shupe, D. L., Soumagnac, M. T., Strotjohann, N. L., Taggart, K., Tartaglia, L., Yan, L., and Zolkower, J.

Abstract

We present optical, radio, and X-ray observations of SN2020bvc (=ASASSN20bs; ZTF20aalxlis), a nearby ($z=0.0252$; $d$=114 Mpc) broad-lined (BL) Type Ic supernova (SN). Our observations show that SN2020bvc shares several properties in common with the Ic-BL SN2006aj, which was associated with the low-luminosity gamma-ray burst (LLGRB) 060218. First, the 10 GHz radio light curve is on the faint end of LLGRB-SNe ($L_\mathrm{radio} \approx 10^{37}$erg/s): we model our VLA observations (spanning 13-43 d) as synchrotron emission from a mildly relativistic ($v \gtrsim 0.3c$) forward shock. Second, with Swift and Chandra we detect X-ray emission ($L_X \approx 10^{41}$erg/s) that is not naturally explained as inverse Compton emission or as part of the same synchrotron spectrum as the radio emission. Third, high-cadence ($6\times$/night) data from the Zwicky Transient Facility (ZTF) shows a double-peaked optical light curve, the first peak from shock-cooling emission from extended low-mass material (mass $M<10^{-2} M_\odot$ at radius $R>10^{12}$cm) and the second peak from the radioactive decay of Ni-56. SN2020bvc is the first confirmed double-peaked Ic-BL SN discovered without a GRB trigger, and shows X-ray and radio emission similar to LLGRB-SNe: this is consistent with models in which the same mechanism produces both the LLGRB and the shock-cooling emission. For four of the five other nearby ($z\lesssim0.05$) Ic-BL SNe with ZTF high-cadence data, we rule out a first peak like that seen in SN2006aj and SN2020bvc, i.e. that lasts $\approx 1$d and reaches a peak luminosity $M \approx -18$. X-ray and radio follow-up observations of future such events will establish whether double-peaked optical light curves are indeed predictive of LLGRB-like X-ray and radio emission., Comment: Accepted to ApJ. 39 pages, 17 figures. Comments welcome

Published
2020
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19. The Koala: A Fast Blue Optical Transient with Luminous Radio Emission from a Starburst Dwarf Galaxy at $z=0.27$

Author

Ho, Anna Y. Q., Perley, D. A., Kulkarni, S. R., Dong, D. Z. J., De, K., Chandra, P., Andreoni, I., Bellm, E. C., Burdge, K. B., Coughlin, M., Dekany, R., Feeney, M., Frederiks, D. D., Fremling, C., Golkhou, V. Z., Graham, M., Hale, D., Helou, G., Horesh, A., Laher, R. R., Masci, F., Miller, A. A., Porter, M., Ridnaia, A., Rusholme, B., Shupe, D. L., Soumagnac, M. T., Svinkin, D. S., Ho, Anna Y. Q., Perley, D. A., Kulkarni, S. R., Dong, D. Z. J., De, K., Chandra, P., Andreoni, I., Bellm, E. C., Burdge, K. B., Coughlin, M., Dekany, R., Feeney, M., Frederiks, D. D., Fremling, C., Golkhou, V. Z., Graham, M., Hale, D., Helou, G., Horesh, A., Laher, R. R., Masci, F., Miller, A. A., Porter, M., Ridnaia, A., Rusholme, B., Shupe, D. L., Soumagnac, M. T., and Svinkin, D. S.

Abstract

We present ZTF18abvkwla (the "Koala"), a fast blue optical transient discovered in the Zwicky Transient Facility (ZTF) One-Day Cadence (1DC) Survey. ZTF18abvkwla has a number of features in common with the groundbreaking transient AT2018cow: blue colors at peak ($g-r\approx-0.5$ mag), a short rise time from half-max of under two days, a decay time to half-max of only three days, a high optical luminosity ($M_{g,\mathrm{peak}}\approx-20.6$mag), a hot ($\gtrsim 40,000$K) featureless spectrum at peak light, and a luminous radio counterpart. At late times ($\Delta t>80$d) the radio luminosity of ZTF18abvkwla ($\nu L_\nu \gtrsim 10^{40}$erg/s at 10 GHz, observer-frame) is most similar to that of long-duration gamma-ray bursts (GRBs). The host galaxy is a dwarf starburst galaxy ($M\approx5\times10^{8}M_\odot$, $\mathrm{SFR}\approx7 M_\odot$/yr) that is moderately metal-enriched ($\log\mathrm{[O/H]} \approx 8.5$), similar to the hosts of GRBs and superluminous supernovae. As in AT2018cow, the radio and optical emission in ZTF18abvkwla likely arise from two separate components: the radio from fast-moving ejecta ($\Gamma \beta c >0.38c$) and the optical from shock-interaction with confined dense material ($<0.07M_\odot$ in $\sim 10^{15}$cm). Compiling transients in the literature with $t_\mathrm{rise} <5$d and $M_\mathrm{peak}<-20$mag, we find that a significant number are engine-powered, and suggest that the high peak optical luminosity is directly related to the presence of this engine. From 18 months of the 1DC survey, we find that transients in this rise-luminosity phase space are at least two to three orders of magnitude less common than CC SNe. Finally, we discuss strategies for identifying such events with future facilities like the Large Synoptic Survey Telescope, and prospects for detecting accompanying X-ray and radio emission., Comment: 27 pages, 11 figures. Resubmitted to ApJ on 13 April following comments by referee. Comments welcome!

Published
2020
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20. ZTF Early Observations of Type Ia Supernovae II: First Light, the Initial Rise, and Time to Reach Maximum Brightness

Author

Miller, A. A., Yao, Y., Bulla, M., Pankow, C., Bellm, E. C., Cenko, S. B., Dekany, R., Fremling, C., Graham, M. J., Kupfer, T., Laher, R. R., Mahabal, A. A., Masci, F. J., Nugent, P. E., Riddle, R., Rusholme, B., Smith, R. M., Shupe, D. L., van Roestel, J., Kulkarni, S. R., Miller, A. A., Yao, Y., Bulla, M., Pankow, C., Bellm, E. C., Cenko, S. B., Dekany, R., Fremling, C., Graham, M. J., Kupfer, T., Laher, R. R., Mahabal, A. A., Masci, F. J., Nugent, P. E., Riddle, R., Rusholme, B., Smith, R. M., Shupe, D. L., van Roestel, J., and Kulkarni, S. R.

Abstract

While it is clear that Type Ia supernovae (SNe) are the result of thermonuclear explosions in C/O white dwarfs (WDs), a great deal remains uncertain about the binary companion that facilitates the explosive disruption of the WD. Here, we present a comprehensive analysis of a large, unique data set of 127 SNe$\,$Ia with exquisite coverage by the Zwicky Transient Facility (ZTF). High-cadence (six observations per night) ZTF observations allow us to measure the SN rise time and examine its initial evolution. We develop a Bayesian framework to model the early rise as a power law in time, which enables the inclusion of priors in our model. For a volume-limited subset of normal SNe$\,$Ia, we find that the mean power-law index is consistent with 2 in the $r_\mathrm{ZTF}$-band ($\alpha_r = 2.01\pm0.02$), as expected in the expanding fireball model. There are, however, individual SNe that are clearly inconsistent with $\alpha_r=2$. We estimate a mean rise time of 18.9$\,$d (with a range extending from $\sim$15 to 22$\,$d), though this is subject to the adopted prior. We identify an important, previously unknown, bias whereby the rise times for higher-redshift SNe within a flux-limited survey are systematically underestimated. This effect can be partially alleviated if the power-law index is fixed to $\alpha=2$, in which case we estimate a mean rise time of 21.7$\,$d (with a range from $\sim$18 to 23$\,$d). The sample includes a handful of rare and peculiar SNe$\,$Ia. Finally, we conclude with a discussion of lessons learned from the ZTF sample that can eventually be applied to observations from the Vera C. Rubin Observatory., Comment: 31 pages, 17 figures; ApJ accepted

Published
2020
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21. The Death Throes of a Stripped Massive Star: An Eruptive Mass-Loss History Encoded in Pre-Explosion Emission, a Rapidly Rising Luminous Transient, and a Broad-Lined Ic Supernova SN2018gep

Author

Ho, Anna Y. Q., Goldstein, Daniel A., Schulze, Steve, Khatami, David K., Perley, D. A., Ergon, Mattias, Gal-Yam, Avishay, Corsi, Alessandra, Andreoni, Igor, Barbarino, Cristina, Bellm, Eric C., Blagorodnova, Nadejda, Bright, Joe S., Burns, Eric, Cenko, S. B., Cunningham, Virginia, De, Kishalay, Dekany, Richard, Dugas, Alison M., Fender, Rob P., Fransson, Claes, Fremling, Christoffer, Goldstein, Adam, Graham, Matthew J., Hale, David, Horesh, Assaf, Hung, Tiara, Kasliwal, Mansi M., Kuin, N. Paul M., Kulkarni, S. R., Kupfer, Thomas, Lunnan, Ragnhild, Masci, Frank J., Ngeow, Chow-Choong, Nugent, Peter E., Ofek, Eran O., Patterson, Maria T., Pettipas, Glen, Rusholme, Ben, Sai, Hanna, Sfaradi, Itai, Shupe, D. L., Sollerman, J., Soumagnac, Maayane T., Tachibana, Yutaro, Taddia, Francesco, Walters, Richard, Wang, Xiaofeng, Yao, Yuhan, Zhang, Xinhan, Ho, Anna Y. Q., Goldstein, Daniel A., Schulze, Steve, Khatami, David K., Perley, D. A., Ergon, Mattias, Gal-Yam, Avishay, Corsi, Alessandra, Andreoni, Igor, Barbarino, Cristina, Bellm, Eric C., Blagorodnova, Nadejda, Bright, Joe S., Burns, Eric, Cenko, S. B., Cunningham, Virginia, De, Kishalay, Dekany, Richard, Dugas, Alison M., Fender, Rob P., Fransson, Claes, Fremling, Christoffer, Goldstein, Adam, Graham, Matthew J., Hale, David, Horesh, Assaf, Hung, Tiara, Kasliwal, Mansi M., Kuin, N. Paul M., Kulkarni, S. R., Kupfer, Thomas, Lunnan, Ragnhild, Masci, Frank J., Ngeow, Chow-Choong, Nugent, Peter E., Ofek, Eran O., Patterson, Maria T., Pettipas, Glen, Rusholme, Ben, Sai, Hanna, Sfaradi, Itai, Shupe, D. L., Sollerman, J., Soumagnac, Maayane T., Tachibana, Yutaro, Taddia, Francesco, Walters, Richard, Wang, Xiaofeng, Yao, Yuhan, and Zhang, Xinhan

Abstract

We present detailed observations of ZTF18abukavn (SN2018gep), discovered in high-cadence data from the Zwicky Transient Facility as a rapidly rising (1.3 mag/hr) and luminous (M_(g,peak) = −20 mag) transient. It is spectroscopically classified as a broad-lined stripped-envelope supernova (Ic-BL SN). The rapid rise to peak bolometric luminosity and blue colors at peak (t_(rise)∼0.5-3 days, L_(bol)≳3×10^(44) erg sec^(−1), g−r = −0.3) resemble the high-redshift Ic-BL iPTF16asu, as well as several other unclassified fast transients. The early discovery of SN2018gep (within an hour of shock breakout) enabled an intensive spectroscopic campaign, including the highest-temperature (T_(eff) ≳ 40,000K) spectra of a stripped-envelope SN. A retrospective search revealed luminous (M_g ∼ M_r ≈ −14mag) emission in the days to weeks before explosion, the first definitive detection of precursor emission for a Ic-BL. We find a limit on the isotropic gamma-ray energy release E_(γ,iso) < 4.9×10^(48) erg, a limit on X-ray emission L_X < 10^(40) erg sec^(−1), and a limit on radio emission νL_ν ≲ 10^(37) erg sec^(−1). Taken together, we find that the data are best explained by shock breakout in a massive shell of dense circumstellar material (0.02 M⊙) at large radii (3×10^(14)cm) that was ejected in eruptive pre-explosion mass-loss episodes.

Published
2019

22. Four (Super)luminous Supernovae from the First Months of the ZTF Survey

Author

Lunnan, R., Yan, Lin, Perley, D. A., Schulze, S., Taggart, K., Gal-Yam, A., Fremling, C., Soumagnac, M. T., Ofek, E., Adams, S. M., Barbarino, C., Bellm, E. C., De, K., Fransson, C., Frederick, S., Golkhou, V. Z., Graham, M. J., Hallakoun, N., Ho, A. Y. Q., Kasliwal, M. M., Kaspi, S., Kulkarni, S. R., Laher, R. R., Masci, F. J., Nunez, F. Pozo, Rusholme, B., Quimby, R. M., Shupe, D. L., Sollerman, J., Taddia, F., van Roestel, J., Yang, Y., Yao, Yuhan, Lunnan, R., Yan, Lin, Perley, D. A., Schulze, S., Taggart, K., Gal-Yam, A., Fremling, C., Soumagnac, M. T., Ofek, E., Adams, S. M., Barbarino, C., Bellm, E. C., De, K., Fransson, C., Frederick, S., Golkhou, V. Z., Graham, M. J., Hallakoun, N., Ho, A. Y. Q., Kasliwal, M. M., Kaspi, S., Kulkarni, S. R., Laher, R. R., Masci, F. J., Nunez, F. Pozo, Rusholme, B., Quimby, R. M., Shupe, D. L., Sollerman, J., Taddia, F., van Roestel, J., Yang, Y., and Yao, Yuhan

Abstract

We present photometry and spectroscopy of four hydrogen-poor luminous supernovae discovered during the two-month science commissioning and early operations of the Zwicky Transient Facility (ZTF) survey. Three of these objects, SN2018bym (ZTF18aapgrxo), SN2018avk (ZTF18aaisyyp) and SN2018bgv (ZTF18aavrmcg) resemble typical SLSN-I spectroscopically, while SN2018don (ZTF18aajqcue) may be an object similar to SN2007bi experiencing considerable host galaxy reddening, or an intrinsically long-lived, luminous and red SN Ic. We analyze the light curves, spectra, and host galaxy properties of these four objects and put them in context of the population of SLSN-I. SN2018bgv stands out as the fastest-rising SLSN-I observed to date, with a rest-frame g-band rise time of just 10 days from explosion to peak -- if it is powered by magnetar spin-down, the implied ejecta mass is only ~1 M$_{\odot}$. SN2018don also displays unusual properties -- in addition to its red colors and comparatively massive host galaxy, the light curve undergoes some of the strongest light curve undulations post-peak seen in a SLSN-I, which we speculate may be due to interaction with circumstellar material. We discuss the promises and challenges of finding SLSNe in large-scale surveys like ZTF given the observed diversity in the population., Comment: Updated to match published version. Expanded discussion following referee comments; conclusions unchanged

Published
2019
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23. Four (Super)luminous Supernovae from the First Months of the ZTF Survey

Author

Lunnan, R., Yan, Lin, Perley, D. A., Schulze, S., Taggart, K., Gal-Yam, A., Fremling, C., Soumagnac, M. T., Ofek, E., Adams, S. M., Barbarino, C., Bellm, E. C., De, K., Fransson, C., Frederick, S., Golkhou, V. Z., Graham, M. J., Hallakoun, N., Ho, A. Y. Q., Kasliwal, M. M., Kaspi, S., Kulkarni, S. R., Laher, R. R., Masci, F. J., Nunez, F. Pozo, Rusholme, B., Quimby, R. M., Shupe, D. L., Sollerman, J., Taddia, F., van Roestel, J., Yang, Y., Yao, Yuhan, Lunnan, R., Yan, Lin, Perley, D. A., Schulze, S., Taggart, K., Gal-Yam, A., Fremling, C., Soumagnac, M. T., Ofek, E., Adams, S. M., Barbarino, C., Bellm, E. C., De, K., Fransson, C., Frederick, S., Golkhou, V. Z., Graham, M. J., Hallakoun, N., Ho, A. Y. Q., Kasliwal, M. M., Kaspi, S., Kulkarni, S. R., Laher, R. R., Masci, F. J., Nunez, F. Pozo, Rusholme, B., Quimby, R. M., Shupe, D. L., Sollerman, J., Taddia, F., van Roestel, J., Yang, Y., and Yao, Yuhan

Abstract

We present photometry and spectroscopy of four hydrogen-poor luminous supernovae discovered during the two-month science commissioning and early operations of the Zwicky Transient Facility (ZTF) survey. Three of these objects, SN2018bym (ZTF18aapgrxo), SN2018avk (ZTF18aaisyyp) and SN2018bgv (ZTF18aavrmcg) resemble typical SLSN-I spectroscopically, while SN2018don (ZTF18aajqcue) may be an object similar to SN2007bi experiencing considerable host galaxy reddening, or an intrinsically long-lived, luminous and red SN Ic. We analyze the light curves, spectra, and host galaxy properties of these four objects and put them in context of the population of SLSN-I. SN2018bgv stands out as the fastest-rising SLSN-I observed to date, with a rest-frame g-band rise time of just 10 days from explosion to peak -- if it is powered by magnetar spin-down, the implied ejecta mass is only ~1 M$_{\odot}$. SN2018don also displays unusual properties -- in addition to its red colors and comparatively massive host galaxy, the light curve undergoes some of the strongest light curve undulations post-peak seen in a SLSN-I, which we speculate may be due to interaction with circumstellar material. We discuss the promises and challenges of finding SLSNe in large-scale surveys like ZTF given the observed diversity in the population., Comment: Updated to match published version. Expanded discussion following referee comments; conclusions unchanged

Published
2019
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24. The Astropy Project: Building an inclusive, open-science project and status of the v2.0 core package

Author

The Astropy Collaboration, Price-Whelan, A. M., Sipőcz, B. M., Günther, H. M., Lim, P. L., Crawford, S. M., Conseil, S., Shupe, D. L., Craig, M. W., Dencheva, N., Ginsburg, A., VanderPlas, J. T., Bradley, L. D., Pérez-Suárez, D., de Val-Borro, M., Aldcroft, T. L., Cruz, K. L., Robitaille, T. P., Tollerud, E. J., Ardelean, C., Babej, T., Bachetti, M., Bakanov, A. V., Bamford, S. P., Barentsen, G., Barmby, P., Baumbach, A., Berry, K. L., Biscani, F., Boquien, M., Bostroem, K. A., Bouma, L. G., Brammer, G. B., Bray, E. M., Breytenbach, H., Buddelmeijer, H., Burke, D. J., Calderone, G., Rodríguez, J. L. Cano, Cara, M., Cardoso, J. V. M., Cheedella, S., Copin, Y., Crichton, D., DÁvella, D., Deil, C., Depagne, É., Dietrich, J. P., Donath, A., Droettboom, M., Earl, N., Erben, T., Fabbro, S., Ferreira, L. A., Finethy, T., Fox, R. T., Garrison, L. H., Gibbons, S. L. J., Goldstein, D. A., Gommers, R., Greco, J. P., Greenfield, P., Groener, A. M., Grollier, F., Hagen, A., Hirst, P., Homeier, D., Horton, A. J., Hosseinzadeh, G., Hu, L., Hunkeler, J. S., Ivezić, Ž., Jain, A., Jenness, T., Kanarek, G., Kendrew, S., Kern, N. S., Kerzendorf, W. E., Khvalko, A., King, J., Kirkby, D., Kulkarni, A. M., Kumar, A., Lee, A., Lenz, D., Littlefair, S. P., Ma, Z., Macleod, D. M., Mastropietro, M., McCully, C., Montagnac, S., Morris, B. M., Mueller, M., Mumford, S. J., Muna, D., Murphy, N. A., Nelson, S., Nguyen, G. H., Ninan, J. P., Nöthe, M., Ogaz, S., Oh, S., Parejko, J. K., Parley, N., Pascual, S., Patil, R., Patil, A. A., Plunkett, A. L., Prochaska, J. X., Rastogi, T., Janga, V. Reddy, Sabater, J., Sakurikar, P., Seifert, M., Sherbert, L. E., Sherwood-Taylor, H., Shih, A. Y., Sick, J., Silbiger, M. T., Singanamalla, S., Singer, L. P., Sladen, P. H., Sooley, K. A., Sornarajah, S., Streicher, O., Teuben, P., Thomas, S. W., Tremblay, G. R., Turner, J. E. H., Terrón, V., van Kerkwijk, M. H., de la Vega, A., Watkins, L. L., Weaver, B. A., Whitmore, J. B., Woillez, J., Zabalza, V., The Astropy Collaboration, Price-Whelan, A. M., Sipőcz, B. M., Günther, H. M., Lim, P. L., Crawford, S. M., Conseil, S., Shupe, D. L., Craig, M. W., Dencheva, N., Ginsburg, A., VanderPlas, J. T., Bradley, L. D., Pérez-Suárez, D., de Val-Borro, M., Aldcroft, T. L., Cruz, K. L., Robitaille, T. P., Tollerud, E. J., Ardelean, C., Babej, T., Bachetti, M., Bakanov, A. V., Bamford, S. P., Barentsen, G., Barmby, P., Baumbach, A., Berry, K. L., Biscani, F., Boquien, M., Bostroem, K. A., Bouma, L. G., Brammer, G. B., Bray, E. M., Breytenbach, H., Buddelmeijer, H., Burke, D. J., Calderone, G., Rodríguez, J. L. Cano, Cara, M., Cardoso, J. V. M., Cheedella, S., Copin, Y., Crichton, D., DÁvella, D., Deil, C., Depagne, É., Dietrich, J. P., Donath, A., Droettboom, M., Earl, N., Erben, T., Fabbro, S., Ferreira, L. A., Finethy, T., Fox, R. T., Garrison, L. H., Gibbons, S. L. J., Goldstein, D. A., Gommers, R., Greco, J. P., Greenfield, P., Groener, A. M., Grollier, F., Hagen, A., Hirst, P., Homeier, D., Horton, A. J., Hosseinzadeh, G., Hu, L., Hunkeler, J. S., Ivezić, Ž., Jain, A., Jenness, T., Kanarek, G., Kendrew, S., Kern, N. S., Kerzendorf, W. E., Khvalko, A., King, J., Kirkby, D., Kulkarni, A. M., Kumar, A., Lee, A., Lenz, D., Littlefair, S. P., Ma, Z., Macleod, D. M., Mastropietro, M., McCully, C., Montagnac, S., Morris, B. M., Mueller, M., Mumford, S. J., Muna, D., Murphy, N. A., Nelson, S., Nguyen, G. H., Ninan, J. P., Nöthe, M., Ogaz, S., Oh, S., Parejko, J. K., Parley, N., Pascual, S., Patil, R., Patil, A. A., Plunkett, A. L., Prochaska, J. X., Rastogi, T., Janga, V. Reddy, Sabater, J., Sakurikar, P., Seifert, M., Sherbert, L. E., Sherwood-Taylor, H., Shih, A. Y., Sick, J., Silbiger, M. T., Singanamalla, S., Singer, L. P., Sladen, P. H., Sooley, K. A., Sornarajah, S., Streicher, O., Teuben, P., Thomas, S. W., Tremblay, G. R., Turner, J. E. H., Terrón, V., van Kerkwijk, M. H., de la Vega, A., Watkins, L. L., Weaver, B. A., Whitmore, J. B., Woillez, J., and Zabalza, V.

Abstract

The Astropy project supports and fosters the development of open-source and openly-developed Python packages that provide commonly-needed functionality to the astronomical community. A key element of the Astropy project is the core package Astropy, which serves as the foundation for more specialized projects and packages. In this article, we provide an overview of the organization of the Astropy project and summarize key features in the core package as of the recent major release, version 2.0. We then describe the project infrastructure designed to facilitate and support development for a broader ecosystem of inter-operable packages. We conclude with a future outlook of planned new features and directions for the broader Astropy project., Comment: Minor changes to author list and title. Comments and feedback welcome through the paper source repository: https://github.com/astropy/astropy-v2.0-paper For more information about Astropy, see http://www.astropy.org

Published
2018
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25. The Astropy Project: Building an Open-science Project and Status of the v2.0 Core Package

Author

Price-Whelan, A. M., Sipocz, B. M., Gunther, H. M., Lim, P. L., Crawford, S. M., Conseil, S., Shupe, D. L., Craig, M. W., Dencheva, N., Ginsburg, A., VanderPlas, J. T., Bradley, L. D., Perez-Suarez, D., de Val-Borro, M., Aldcroft, T. L., Cruz, K. L., Robitaille, T. P., Tollerud, E. J., Ardelean, C., Babej, T., Bach, Y. P., Bachetti, M., Bakanov, A. V., Bamford, S. P., Barentsen, G., Barmby, P., Baumbach, A., Berry, K. L., Biscani, F., Boquien, M., Bostroem, K. A., Bouma, L. G., Brammer, G. B., Bray, E. M., Breytenbach, H., Buddelmeijer, H., Burke, D. J., Calderone, G., Cano Rodriguez, J. L., Cara, M., Cardoso, J. V. M., Cheedella, S., Copin, Y., Corrales, L., Crichton, D., D'Avella, D., Deil, C., Depagne, E., Dietrich, J. P., Donath, A., Droettboom, M., Earl, N., Erben, T., Fabbro, S., Ferreira, L. A., Finethy, T., Fox, R. T., Garrison, L. H., Gibbons, S. L. J., Goldstein, D. A., Gommers, R., Greco, J. P., Greenfield, P., Groener, A. M., Grollier, F., Hagen, A., Hirst, P., Homeier, D., Horton, A. J., Hosseinzadeh, G., Hu, L., Hunkeler, J. S., Ivezic, Z., Jain, A., Jenness, T., Kanarek, G., Kendrew, S., Kern, N. S., Kerzendorf, W. E., Khvalko, A., King, J., Kirkby, D., Kulkarni, A. M., Kumar, A., Lee, A., Lenz, D., Littlefair, S. P., Ma, Z., Macleod, D. M., Mastropietro, M., McCully, C., Montagnac, S., Morris, B. M., Mueller, M., Mumford, S. J., Muna, D., Murphy, N. A., Nelson, S., Nguyen, G. H., Ninan, J. P., Noethe, M., Ogaz, S., Oh, S., Parejko, J. K., Parley, N., Pascual, S., Patil, R., Patil, A. A., Plunkett, A. L., Prochaska, J. X., Rastogi, T., Janga, V. Reddy, Sabater, J., Sakurikar, P., Seifert, M., Sherbert, L. E., Sherwood-Taylor, H., Shih, A. Y., Sick, J., Silbiger, M. T., Singanamalla, S., Singer, L. P., Sladen, P. H., Sooley, K. A., Sornarajah, S., Streicher, O., Teuben, P., Thomas, S. W., Tremblay, G. R., Turner, J. E. H., Terron, V., van Kerkwijk, M. H., de la Vegat, A., Watkins, L. L., Weaver, B. A., Whitmore, J. B., Woillez, J., Zabalza, V., Price-Whelan, A. M., Sipocz, B. M., Gunther, H. M., Lim, P. L., Crawford, S. M., Conseil, S., Shupe, D. L., Craig, M. W., Dencheva, N., Ginsburg, A., VanderPlas, J. T., Bradley, L. D., Perez-Suarez, D., de Val-Borro, M., Aldcroft, T. L., Cruz, K. L., Robitaille, T. P., Tollerud, E. J., Ardelean, C., Babej, T., Bach, Y. P., Bachetti, M., Bakanov, A. V., Bamford, S. P., Barentsen, G., Barmby, P., Baumbach, A., Berry, K. L., Biscani, F., Boquien, M., Bostroem, K. A., Bouma, L. G., Brammer, G. B., Bray, E. M., Breytenbach, H., Buddelmeijer, H., Burke, D. J., Calderone, G., Cano Rodriguez, J. L., Cara, M., Cardoso, J. V. M., Cheedella, S., Copin, Y., Corrales, L., Crichton, D., D'Avella, D., Deil, C., Depagne, E., Dietrich, J. P., Donath, A., Droettboom, M., Earl, N., Erben, T., Fabbro, S., Ferreira, L. A., Finethy, T., Fox, R. T., Garrison, L. H., Gibbons, S. L. J., Goldstein, D. A., Gommers, R., Greco, J. P., Greenfield, P., Groener, A. M., Grollier, F., Hagen, A., Hirst, P., Homeier, D., Horton, A. J., Hosseinzadeh, G., Hu, L., Hunkeler, J. S., Ivezic, Z., Jain, A., Jenness, T., Kanarek, G., Kendrew, S., Kern, N. S., Kerzendorf, W. E., Khvalko, A., King, J., Kirkby, D., Kulkarni, A. M., Kumar, A., Lee, A., Lenz, D., Littlefair, S. P., Ma, Z., Macleod, D. M., Mastropietro, M., McCully, C., Montagnac, S., Morris, B. M., Mueller, M., Mumford, S. J., Muna, D., Murphy, N. A., Nelson, S., Nguyen, G. H., Ninan, J. P., Noethe, M., Ogaz, S., Oh, S., Parejko, J. K., Parley, N., Pascual, S., Patil, R., Patil, A. A., Plunkett, A. L., Prochaska, J. X., Rastogi, T., Janga, V. Reddy, Sabater, J., Sakurikar, P., Seifert, M., Sherbert, L. E., Sherwood-Taylor, H., Shih, A. Y., Sick, J., Silbiger, M. T., Singanamalla, S., Singer, L. P., Sladen, P. H., Sooley, K. A., Sornarajah, S., Streicher, O., Teuben, P., Thomas, S. W., Tremblay, G. R., Turner, J. E. H., Terron, V., van Kerkwijk, M. H., de la Vegat, A., Watkins, L. L., Weaver, B. A., Whitmore, J. B., Woillez, J., and Zabalza, V.

Abstract

The Astropy Project supports and fosters the development of open-source and openly developed Python packages that provide commonly needed functionality to the astronomical community. A key element of the Astropy Project is the core package astropy, which serves as the foundation for more specialized projects and packages. In this article, we provide an overview of the organization of the Astropy project and summarize key features in the core package, as of the recent major release, version 2.0. We then describe the project infrastructure designed to facilitate and support development for a broader ecosystem of interoperable packages. We conclude with a future outlook of planned new features and directions for the broader Astropy Project.

Published
2018
Full Text
View/download PDF

26. The Astropy Project: Building an Open-science Project and Status of the v2.0 Core Package

Author

Physics, Price-Whelan, A. M., Sipocz, B. M., Gunther, H. M., Lim, P. L., Crawford, S. M., Conseil, S., Shupe, D. L., Craig, M. W., Dencheva, N., Ginsburg, A., VanderPlas, J. T., Bradley, L. D., Perez-Suarez, D., de Val-Borro, M., Aldcroft, T. L., Cruz, K. L., Robitaille, T. P., Tollerud, E. J., Ardelean, C., Babej, T., Bach, Y. P., Bachetti, M., Bakanov, A. V., Bamford, S. P., Barentsen, G., Barmby, P., Baumbach, A., Berry, K. L., Biscani, F., Boquien, M., Bostroem, K. A., Bouma, L. G., Brammer, G. B., Bray, E. M., Breytenbach, H., Buddelmeijer, H., Burke, D. J., Calderone, G., Cano Rodriguez, J. L., Cara, M., Cardoso, J. V. M., Cheedella, S., Copin, Y., Corrales, L., Crichton, D., D'Avella, D., Deil, C., Depagne, E., Dietrich, J. P., Donath, A., Droettboom, M., Earl, N., Erben, T., Fabbro, S., Ferreira, L. A., Finethy, T., Fox, R. T., Garrison, L. H., Gibbons, S. L. J., Goldstein, D. A., Gommers, R., Greco, J. P., Greenfield, P., Groener, A. M., Grollier, F., Hagen, A., Hirst, P., Homeier, D., Horton, A. J., Hosseinzadeh, G., Hu, L., Hunkeler, J. S., Ivezic, Z., Jain, A., Jenness, T., Kanarek, G., Kendrew, S., Kern, N. S., Kerzendorf, W. E., Khvalko, A., King, J., Kirkby, D., Kulkarni, A. M., Kumar, A., Lee, A., Lenz, D., Littlefair, S. P., Ma, Z., Macleod, D. M., Mastropietro, M., McCully, C., Montagnac, S., Morris, B. M., Mueller, M., Mumford, S. J., Muna, D., Murphy, N. A., Nelson, S., Nguyen, G. H., Ninan, J. P., Noethe, M., Ogaz, S., Oh, S., Parejko, J. K., Parley, N., Pascual, S., Patil, R., Patil, A. A., Plunkett, A. L., Prochaska, J. X., Rastogi, T., Janga, V. Reddy, Sabater, J., Sakurikar, P., Seifert, M., Sherbert, L. E., Sherwood-Taylor, H., Shih, A. Y., Sick, J., Silbiger, M. T., Singanamalla, S., Singer, L. P., Sladen, P. H., Sooley, K. A., Sornarajah, S., Streicher, O., Teuben, P., Thomas, S. W., Tremblay, G. R., Turner, J. E. H., Terron, V., van Kerkwijk, M. H., de la Vegat, A., Watkins, L. L., Weaver, B. A., Whitmore, J. B., Woillez, J., Zabalza, V., Physics, Price-Whelan, A. M., Sipocz, B. M., Gunther, H. M., Lim, P. L., Crawford, S. M., Conseil, S., Shupe, D. L., Craig, M. W., Dencheva, N., Ginsburg, A., VanderPlas, J. T., Bradley, L. D., Perez-Suarez, D., de Val-Borro, M., Aldcroft, T. L., Cruz, K. L., Robitaille, T. P., Tollerud, E. J., Ardelean, C., Babej, T., Bach, Y. P., Bachetti, M., Bakanov, A. V., Bamford, S. P., Barentsen, G., Barmby, P., Baumbach, A., Berry, K. L., Biscani, F., Boquien, M., Bostroem, K. A., Bouma, L. G., Brammer, G. B., Bray, E. M., Breytenbach, H., Buddelmeijer, H., Burke, D. J., Calderone, G., Cano Rodriguez, J. L., Cara, M., Cardoso, J. V. M., Cheedella, S., Copin, Y., Corrales, L., Crichton, D., D'Avella, D., Deil, C., Depagne, E., Dietrich, J. P., Donath, A., Droettboom, M., Earl, N., Erben, T., Fabbro, S., Ferreira, L. A., Finethy, T., Fox, R. T., Garrison, L. H., Gibbons, S. L. J., Goldstein, D. A., Gommers, R., Greco, J. P., Greenfield, P., Groener, A. M., Grollier, F., Hagen, A., Hirst, P., Homeier, D., Horton, A. J., Hosseinzadeh, G., Hu, L., Hunkeler, J. S., Ivezic, Z., Jain, A., Jenness, T., Kanarek, G., Kendrew, S., Kern, N. S., Kerzendorf, W. E., Khvalko, A., King, J., Kirkby, D., Kulkarni, A. M., Kumar, A., Lee, A., Lenz, D., Littlefair, S. P., Ma, Z., Macleod, D. M., Mastropietro, M., McCully, C., Montagnac, S., Morris, B. M., Mueller, M., Mumford, S. J., Muna, D., Murphy, N. A., Nelson, S., Nguyen, G. H., Ninan, J. P., Noethe, M., Ogaz, S., Oh, S., Parejko, J. K., Parley, N., Pascual, S., Patil, R., Patil, A. A., Plunkett, A. L., Prochaska, J. X., Rastogi, T., Janga, V. Reddy, Sabater, J., Sakurikar, P., Seifert, M., Sherbert, L. E., Sherwood-Taylor, H., Shih, A. Y., Sick, J., Silbiger, M. T., Singanamalla, S., Singer, L. P., Sladen, P. H., Sooley, K. A., Sornarajah, S., Streicher, O., Teuben, P., Thomas, S. W., Tremblay, G. R., Turner, J. E. H., Terron, V., van Kerkwijk, M. H., de la Vegat, A., Watkins, L. L., Weaver, B. A., Whitmore, J. B., Woillez, J., and Zabalza, V.

Abstract

The Astropy Project supports and fosters the development of open-source and openly developed Python packages that provide commonly needed functionality to the astronomical community. A key element of the Astropy Project is the core package astropy, which serves as the foundation for more specialized projects and packages. In this article, we provide an overview of the organization of the Astropy project and summarize key features in the core package, as of the recent major release, version 2.0. We then describe the project infrastructure designed to facilitate and support development for a broader ecosystem of interoperable packages. We conclude with a future outlook of planned new features and directions for the broader Astropy Project.

Published
2018

27. The Astropy Project: Building an inclusive, open-science project and status of the v2.0 core package

Author

The Astropy Collaboration, Price-Whelan, A. M., Sipőcz, B. M., Günther, H. M., Lim, P. L., Crawford, S. M., Conseil, S., Shupe, D. L., Craig, M. W., Dencheva, N., Ginsburg, A., VanderPlas, J. T., Bradley, L. D., Pérez-Suárez, D., de Val-Borro, M., Aldcroft, T. L., Cruz, K. L., Robitaille, T. P., Tollerud, E. J., Ardelean, C., Babej, T., Bachetti, M., Bakanov, A. V., Bamford, S. P., Barentsen, G., Barmby, P., Baumbach, A., Berry, K. L., Biscani, F., Boquien, M., Bostroem, K. A., Bouma, L. G., Brammer, G. B., Bray, E. M., Breytenbach, H., Buddelmeijer, H., Burke, D. J., Calderone, G., Rodríguez, J. L. Cano, Cara, M., Cardoso, J. V. M., Cheedella, S., Copin, Y., Crichton, D., DÁvella, D., Deil, C., Depagne, É., Dietrich, J. P., Donath, A., Droettboom, M., Earl, N., Erben, T., Fabbro, S., Ferreira, L. A., Finethy, T., Fox, R. T., Garrison, L. H., Gibbons, S. L. J., Goldstein, D. A., Gommers, R., Greco, J. P., Greenfield, P., Groener, A. M., Grollier, F., Hagen, A., Hirst, P., Homeier, D., Horton, A. J., Hosseinzadeh, G., Hu, L., Hunkeler, J. S., Ivezić, Ž., Jain, A., Jenness, T., Kanarek, G., Kendrew, S., Kern, N. S., Kerzendorf, W. E., Khvalko, A., King, J., Kirkby, D., Kulkarni, A. M., Kumar, A., Lee, A., Lenz, D., Littlefair, S. P., Ma, Z., Macleod, D. M., Mastropietro, M., McCully, C., Montagnac, S., Morris, B. M., Mueller, M., Mumford, S. J., Muna, D., Murphy, N. A., Nelson, S., Nguyen, G. H., Ninan, J. P., Nöthe, M., Ogaz, S., Oh, S., Parejko, J. K., Parley, N., Pascual, S., Patil, R., Patil, A. A., Plunkett, A. L., Prochaska, J. X., Rastogi, T., Janga, V. Reddy, Sabater, J., Sakurikar, P., Seifert, M., Sherbert, L. E., Sherwood-Taylor, H., Shih, A. Y., Sick, J., Silbiger, M. T., Singanamalla, S., Singer, L. P., Sladen, P. H., Sooley, K. A., Sornarajah, S., Streicher, O., Teuben, P., Thomas, S. W., Tremblay, G. R., Turner, J. E. H., Terrón, V., van Kerkwijk, M. H., de la Vega, A., Watkins, L. L., Weaver, B. A., Whitmore, J. B., Woillez, J., Zabalza, V., The Astropy Collaboration, Price-Whelan, A. M., Sipőcz, B. M., Günther, H. M., Lim, P. L., Crawford, S. M., Conseil, S., Shupe, D. L., Craig, M. W., Dencheva, N., Ginsburg, A., VanderPlas, J. T., Bradley, L. D., Pérez-Suárez, D., de Val-Borro, M., Aldcroft, T. L., Cruz, K. L., Robitaille, T. P., Tollerud, E. J., Ardelean, C., Babej, T., Bachetti, M., Bakanov, A. V., Bamford, S. P., Barentsen, G., Barmby, P., Baumbach, A., Berry, K. L., Biscani, F., Boquien, M., Bostroem, K. A., Bouma, L. G., Brammer, G. B., Bray, E. M., Breytenbach, H., Buddelmeijer, H., Burke, D. J., Calderone, G., Rodríguez, J. L. Cano, Cara, M., Cardoso, J. V. M., Cheedella, S., Copin, Y., Crichton, D., DÁvella, D., Deil, C., Depagne, É., Dietrich, J. P., Donath, A., Droettboom, M., Earl, N., Erben, T., Fabbro, S., Ferreira, L. A., Finethy, T., Fox, R. T., Garrison, L. H., Gibbons, S. L. J., Goldstein, D. A., Gommers, R., Greco, J. P., Greenfield, P., Groener, A. M., Grollier, F., Hagen, A., Hirst, P., Homeier, D., Horton, A. J., Hosseinzadeh, G., Hu, L., Hunkeler, J. S., Ivezić, Ž., Jain, A., Jenness, T., Kanarek, G., Kendrew, S., Kern, N. S., Kerzendorf, W. E., Khvalko, A., King, J., Kirkby, D., Kulkarni, A. M., Kumar, A., Lee, A., Lenz, D., Littlefair, S. P., Ma, Z., Macleod, D. M., Mastropietro, M., McCully, C., Montagnac, S., Morris, B. M., Mueller, M., Mumford, S. J., Muna, D., Murphy, N. A., Nelson, S., Nguyen, G. H., Ninan, J. P., Nöthe, M., Ogaz, S., Oh, S., Parejko, J. K., Parley, N., Pascual, S., Patil, R., Patil, A. A., Plunkett, A. L., Prochaska, J. X., Rastogi, T., Janga, V. Reddy, Sabater, J., Sakurikar, P., Seifert, M., Sherbert, L. E., Sherwood-Taylor, H., Shih, A. Y., Sick, J., Silbiger, M. T., Singanamalla, S., Singer, L. P., Sladen, P. H., Sooley, K. A., Sornarajah, S., Streicher, O., Teuben, P., Thomas, S. W., Tremblay, G. R., Turner, J. E. H., Terrón, V., van Kerkwijk, M. H., de la Vega, A., Watkins, L. L., Weaver, B. A., Whitmore, J. B., Woillez, J., and Zabalza, V.

Abstract

The Astropy project supports and fosters the development of open-source and openly-developed Python packages that provide commonly-needed functionality to the astronomical community. A key element of the Astropy project is the core package Astropy, which serves as the foundation for more specialized projects and packages. In this article, we provide an overview of the organization of the Astropy project and summarize key features in the core package as of the recent major release, version 2.0. We then describe the project infrastructure designed to facilitate and support development for a broader ecosystem of inter-operable packages. We conclude with a future outlook of planned new features and directions for the broader Astropy project., Comment: Minor changes to author list and title. Comments and feedback welcome through the paper source repository: https://github.com/astropy/astropy-v2.0-paper For more information about Astropy, see http://www.astropy.org

Published
2018
Full Text
View/download PDF

28. The Astropy Project: Building an Open-science Project and Status of the v2.0 Core Package

Author

Google, NumFOCUS, Space Telescope Science Institute (US), Harvard-Smithsonian Center for Astrophysics, South African Astronomical Observatory, National Aeronautics and Space Administration (US), Gordon and Betty Moore Foundation, Alfred P. Sloan Foundation, Washington Research Foundation, German Research Foundation, Gemini Observatory, Korea Astronomy and Space Science Institute, Ministerio de Economía y Competitividad (España), European Commission, Price-Whelan, Adrian M., Sipőcz, B. M., Günther, H.M., Lim, P. L., Crawford, S. M., Conseil, S., Shupe, D. L., Craig, M. W., Dencheva, N., Ginsburg, Adam, VanderPlas, J. T., Burke, D. J., Calderone, G., Cano Rodríguez, J. L., Cara, M., Cardoso, J. V. M., Cheedella, S., Copin, Y., Corrales, L., Groener, A. M., Crichton, D., Jenness, T., D'Avella, D., Deil, C., Depagne, É., Dietrich, J. P., Donath, A., Droettboom, M., Earl, N., Erben, T., Fabbro, S., Grollier, F., Kanarek, G., Ferreira, L. A., Finethy, T., Fox, R. T., Garrison, L. H., Gibbons, S. L. J., Goldstein, D. A., Gommers, R., Greco, J. P., Hagen, A., Hirst, P., Kendrew, S., Homeier, D., Horton, A. J., Hosseinzadeh, Griffin, Hu, L., Hunkeler, J. S., Nöthe, M., Ivezić, Ž., Jain, A., Kern, N. S., Kerzendorf, W.E., Khvalko, A., King, J., Kirkby, D., Ogaz, S., Kulkarni, A. M., Sabater, J., Kumar, A., Lee, A., Lenz, D., Littlefair, S. P., Ma, Z., Macleod, D. M., Mastropietro, M., McCully, C., Montagnac, S., Oh, S., Sakurikar, P., Morris, B. M., Mueller, M., Mumford, S. J., Muna, D., Murphy, N. A., Nelson, S., Nguyen, G. H., Ninan, J. P., Parejko, J. K., Parley, N., Seifert, M., Pascual, S., Patil, R., Patil, A. A., Plunkett, A. L., Prochaska, J. Xavier, Bradley, L.D., Rastogi, T., Reddy Janga, V., Sherbert, L. E., Sherwood-Taylor, H., Shih, A. Y., Sick, J., Silbiger, M. T., Pérez-Suárez, D., Singanamalla, S., Barentsen, G., Singer, L. P., Sladen, P. H., Sooley, K. A., Sornarajah, S., Streicher, O., Teuben, P., Thomas, S. W., Tremblay, G. R., Turner, J. E. H., de Val-Borro, M., Barmby, P., Terrón, V., van Kerkwijk, M. H., de la Vega, A., Watkins, L. L., Weaver, B. A., Whitmore, J. B., Woillez, J., Zabalza, V., Aldcroft, T. L., Cruz, Kelle, Baumbach, A., Robitaille, T. P., Tollerud, E. J., Ardelean, C., Babej, T., Bach, Y. P., Bachetti, M., Bakanov, A. V., Bamford, S. P., Berry, K. L., Biscani, F., Boquien, Médéric, Bostroem, K. Azalee, Bouma, L.G., Brammer, G. B., Bray, E. M., Greenfield, P., Breytenbach, H., Buddelmeijer, H., Google, NumFOCUS, Space Telescope Science Institute (US), Harvard-Smithsonian Center for Astrophysics, South African Astronomical Observatory, National Aeronautics and Space Administration (US), Gordon and Betty Moore Foundation, Alfred P. Sloan Foundation, Washington Research Foundation, German Research Foundation, Gemini Observatory, Korea Astronomy and Space Science Institute, Ministerio de Economía y Competitividad (España), European Commission, Price-Whelan, Adrian M., Sipőcz, B. M., Günther, H.M., Lim, P. L., Crawford, S. M., Conseil, S., Shupe, D. L., Craig, M. W., Dencheva, N., Ginsburg, Adam, VanderPlas, J. T., Burke, D. J., Calderone, G., Cano Rodríguez, J. L., Cara, M., Cardoso, J. V. M., Cheedella, S., Copin, Y., Corrales, L., Groener, A. M., Crichton, D., Jenness, T., D'Avella, D., Deil, C., Depagne, É., Dietrich, J. P., Donath, A., Droettboom, M., Earl, N., Erben, T., Fabbro, S., Grollier, F., Kanarek, G., Ferreira, L. A., Finethy, T., Fox, R. T., Garrison, L. H., Gibbons, S. L. J., Goldstein, D. A., Gommers, R., Greco, J. P., Hagen, A., Hirst, P., Kendrew, S., Homeier, D., Horton, A. J., Hosseinzadeh, Griffin, Hu, L., Hunkeler, J. S., Nöthe, M., Ivezić, Ž., Jain, A., Kern, N. S., Kerzendorf, W.E., Khvalko, A., King, J., Kirkby, D., Ogaz, S., Kulkarni, A. M., Sabater, J., Kumar, A., Lee, A., Lenz, D., Littlefair, S. P., Ma, Z., Macleod, D. M., Mastropietro, M., McCully, C., Montagnac, S., Oh, S., Sakurikar, P., Morris, B. M., Mueller, M., Mumford, S. J., Muna, D., Murphy, N. A., Nelson, S., Nguyen, G. H., Ninan, J. P., Parejko, J. K., Parley, N., Seifert, M., Pascual, S., Patil, R., Patil, A. A., Plunkett, A. L., Prochaska, J. Xavier, Bradley, L.D., Rastogi, T., Reddy Janga, V., Sherbert, L. E., Sherwood-Taylor, H., Shih, A. Y., Sick, J., Silbiger, M. T., Pérez-Suárez, D., Singanamalla, S., Barentsen, G., Singer, L. P., Sladen, P. H., Sooley, K. A., Sornarajah, S., Streicher, O., Teuben, P., Thomas, S. W., Tremblay, G. R., Turner, J. E. H., de Val-Borro, M., Barmby, P., Terrón, V., van Kerkwijk, M. H., de la Vega, A., Watkins, L. L., Weaver, B. A., Whitmore, J. B., Woillez, J., Zabalza, V., Aldcroft, T. L., Cruz, Kelle, Baumbach, A., Robitaille, T. P., Tollerud, E. J., Ardelean, C., Babej, T., Bach, Y. P., Bachetti, M., Bakanov, A. V., Bamford, S. P., Berry, K. L., Biscani, F., Boquien, Médéric, Bostroem, K. Azalee, Bouma, L.G., Brammer, G. B., Bray, E. M., Greenfield, P., Breytenbach, H., and Buddelmeijer, H.

Abstract

The Astropy Project supports and fosters the development of open-source and openly developed Python packages that provide commonly needed functionality to the astronomical community. A key element of the Astropy Project is the core package astropy, which serves as the foundation for more specialized projects and packages. In this article, we provide an overview of the organization of the Astropy project and summarize key features in the core package, as of the recent major release, version 2.0. We then describe the project infrastructure designed to facilitate and support development for a broader ecosystem of interoperable packages. We conclude with a future outlook of planned new features and directions for the broader Astropy Project.© 2018. The American Astronomical Society.

Published
2018

29. Discovery of 36 eclipsing EL CVn binaries found by the Palomar Transient Factory

Author

van Roestel, J., Kupfer, T., Ruiz-Carmona, R., Groot, P. J., Prince, T. A., Burdge, K., Laher, R., Shupe, D. L., Bellm, E., van Roestel, J., Kupfer, T., Ruiz-Carmona, R., Groot, P. J., Prince, T. A., Burdge, K., Laher, R., Shupe, D. L., and Bellm, E.

Abstract

We report the discovery and analysis of 36 new eclipsing EL CVn-type binaries, consisting of a core helium-composition pre-white dwarf and an early-type main-sequence companion, more than doubling the known population of these systems. We have used supervised machine learning methods to search 0.8 million lightcurves from the Palomar Transient Factory, combined with SDSS, Pan-STARRS and 2MASS colours. The new systems range in orbital periods from 0.46-3.8 d and in apparent brightness from ~14-16 mag in the PTF $R$ or $g^{\prime}$ filters. For twelve of the systems, we obtained radial velocity curves with the Intermediate Dispersion Spectrograph at the Isaac Newton Telescope. We modelled the lightcurves, radial velocity curves and spectral energy distributions to determine the system parameters. The radii (0.3-0.7 $\mathrm{R_{\odot}}$) and effective temperatures (8000-17000 K) of the pre-He-WDs are consistent with stellar evolution models, but the masses (0.12-0.28 $\mathrm{M_{\odot}}$) show more variance than models predicted. This study shows that using machine learning techniques on large synoptic survey data is a powerful way to discover substantial samples of binary systems in short-lived evolutionary stages.

Published
2017
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30. Discovery of 36 eclipsing EL CVn binaries found by the Palomar Transient Factory

Author

van Roestel, J., Kupfer, T., Ruiz-Carmona, R., Groot, P. J., Prince, T. A., Burdge, K., Laher, R., Shupe, D. L., Bellm, E., van Roestel, J., Kupfer, T., Ruiz-Carmona, R., Groot, P. J., Prince, T. A., Burdge, K., Laher, R., Shupe, D. L., and Bellm, E.

Abstract

We report the discovery and analysis of 36 new eclipsing EL CVn-type binaries, consisting of a core helium-composition pre-white dwarf and an early-type main-sequence companion, more than doubling the known population of these systems. We have used supervised machine learning methods to search 0.8 million lightcurves from the Palomar Transient Factory, combined with SDSS, Pan-STARRS and 2MASS colours. The new systems range in orbital periods from 0.46-3.8 d and in apparent brightness from ~14-16 mag in the PTF $R$ or $g^{\prime}$ filters. For twelve of the systems, we obtained radial velocity curves with the Intermediate Dispersion Spectrograph at the Isaac Newton Telescope. We modelled the lightcurves, radial velocity curves and spectral energy distributions to determine the system parameters. The radii (0.3-0.7 $\mathrm{R_{\odot}}$) and effective temperatures (8000-17000 K) of the pre-He-WDs are consistent with stellar evolution models, but the masses (0.12-0.28 $\mathrm{M_{\odot}}$) show more variance than models predicted. This study shows that using machine learning techniques on large synoptic survey data is a powerful way to discover substantial samples of binary systems in short-lived evolutionary stages.

Published
2017
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31. The HerMES submillimetre local and low-redshift luminosity functions

Author

Marchetti, Lucia, Vaccari, M., Franceschini, A., Arumugam, V., Aussel, H., Bethermin, M., Bock, J., Boselli, A., Buat, V., Burgarella, D., Clements, D.L., Conley, A., Conversi, L., Cooray, A., Dowell, C. D., Farrah, D., Feltre, A., Glenn, J., Griffin, M. J., Hatziminaoglou, E., Heinis, S., Ibar, E., Ivison, R J, Nguyen, H. T., O'Halloran, B., Oliver, S.J., Page, M. J., Papageorgiou, A., Pearson, C. P., Perez-Fournon, I., Pohlen, M., Rigopoulou, D., Roseboom, I.G., Rowan-Robinson, Michael, Schulz, B., Scott, Douglas, Seymour, N, Shupe, D. L., Smith, A. J., Symeonidis, M., Valtchanov, Ivan, Viero, M., Wang, L., Wardlow, J., Xu, C. K., Zemcov, M., Marchetti, Lucia, Vaccari, M., Franceschini, A., Arumugam, V., Aussel, H., Bethermin, M., Bock, J., Boselli, A., Buat, V., Burgarella, D., Clements, D.L., Conley, A., Conversi, L., Cooray, A., Dowell, C. D., Farrah, D., Feltre, A., Glenn, J., Griffin, M. J., Hatziminaoglou, E., Heinis, S., Ibar, E., Ivison, R J, Nguyen, H. T., O'Halloran, B., Oliver, S.J., Page, M. J., Papageorgiou, A., Pearson, C. P., Perez-Fournon, I., Pohlen, M., Rigopoulou, D., Roseboom, I.G., Rowan-Robinson, Michael, Schulz, B., Scott, Douglas, Seymour, N, Shupe, D. L., Smith, A. J., Symeonidis, M., Valtchanov, Ivan, Viero, M., Wang, L., Wardlow, J., Xu, C. K., and Zemcov, M.

Published
2016

32. The HerMES sub-millimetre local and low-redshift luminosity functions

Author

Marchetti, L., Vaccari, M., Franceschini, A., Arumugam, V., Aussel, H., Bethermin, M., Bock, J., Boselli, A., Buat, V., Burgarella, D., Clements, D. L., Conley, A., Conversi, L., Cooray, A., Dowell, C. D., Farrah, D., Feltre, A., Glenn, J., Griffin, M., Hatziminaoglou, E., Heinis, S., Ibar, E., Ivison, R. J., Nguyen, H. T., O'Halloran, B., Oliver, S. J., Omont, A., Page, M. J., Papageorgiou, A., Pearson, C. P., Perez-Fournon, I., Pohlen, M., Rigopoulou, D., Roseboom, I. G., Rowan-Robinson, M., Schulz, B., Scott, Douglas, Seymour, N., Shupe, D. L., Smith, A. J., Symeonidis, M., Valtchanov, I., Viero, M., Wang, L., Wardlow, J., Xu, C. K., Zemcov, M., Marchetti, L., Vaccari, M., Franceschini, A., Arumugam, V., Aussel, H., Bethermin, M., Bock, J., Boselli, A., Buat, V., Burgarella, D., Clements, D. L., Conley, A., Conversi, L., Cooray, A., Dowell, C. D., Farrah, D., Feltre, A., Glenn, J., Griffin, M., Hatziminaoglou, E., Heinis, S., Ibar, E., Ivison, R. J., Nguyen, H. T., O'Halloran, B., Oliver, S. J., Omont, A., Page, M. J., Papageorgiou, A., Pearson, C. P., Perez-Fournon, I., Pohlen, M., Rigopoulou, D., Roseboom, I. G., Rowan-Robinson, M., Schulz, B., Scott, Douglas, Seymour, N., Shupe, D. L., Smith, A. J., Symeonidis, M., Valtchanov, I., Viero, M., Wang, L., Wardlow, J., Xu, C. K., and Zemcov, M.

Abstract

We used wide area surveys over 39 deg$^2$ by the HerMES collaboration, performed with the Herschel Observatory SPIRE multi-wavelength camera, to estimate the low-redshift, $0.02

Published
2015
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33. The Phase Space of z~1.2 SpARCS Clusters: Using Herschel to probe Dust Temperature as a Function of Environment and Accretion History

Author

Noble, A. G., Webb, T. M. A., Yee, H. K. C., Muzzin, A., Wilson, G., van der Burg, R. F. J., Balogh, M. L., Shupe, D. L., Noble, A. G., Webb, T. M. A., Yee, H. K. C., Muzzin, A., Wilson, G., van der Burg, R. F. J., Balogh, M. L., and Shupe, D. L.

Abstract

We present a five-band Herschel study (100-500um) of three galaxy clusters at z~1.2 from the Spitzer Adaptation of the Red-Sequence Cluster Survey (SpARCS). With a sample of 120 spectroscopically-confirmed cluster members, we investigate the role of environment on galaxy properties utilizing the projected cluster phase space (line-of-sight velocity versus clustercentric radius), which probes the time-averaged galaxy density to which a galaxy has been exposed. We divide cluster galaxies into phase-space bins of (r/r200) x (v/sigma_v), tracing a sequence of accretion histories in phase space. Stacking optically star-forming cluster members on the Herschel maps, we measure average infrared star formation rates, and, for the first time in high-redshift galaxy clusters, dust temperatures for dynamically distinct galaxy populations---namely, recent infalls and those that were accreted onto the cluster at an earlier epoch. Proceeding from the infalling to virialized (central) regions of phase space, we find a steady decrease in the specific star formation rate and increase in the stellar age of star-forming cluster galaxies. We perform a probability analysis to investigate all acceptable infrared spectral energy distributions within the full parameter space and measure a ~4 sigma drop in the average dust temperature of cluster galaxies in an intermediate phase-space bin, compared to an otherwise flat trend with phase space. We suggest one plausible quenching mechanism which may be consistent with these trends, invoking ram-pressure stripping of the warmer dust for galaxies within this intermediate accretion phase., Comment: 14 pages, 7 figures, 2 tables; accepted for publication in ApJ

Published
2015
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34. The HerMES sub-millimetre local and low-redshift luminosity functions

Author

Marchetti, L., Vaccari, M., Franceschini, A., Arumugam, V., Aussel, H., Bethermin, M., Bock, J., Boselli, A., Buat, V., Burgarella, D., Clements, D. L., Conley, A., Conversi, L., Cooray, A., Dowell, C. D., Farrah, D., Feltre, A., Glenn, J., Griffin, M., Hatziminaoglou, E., Heinis, S., Ibar, E., Ivison, R. J., Nguyen, H. T., O'Halloran, B., Oliver, S. J., Omont, A., Page, M. J., Papageorgiou, A., Pearson, C. P., Perez-Fournon, I., Pohlen, M., Rigopoulou, D., Roseboom, I. G., Rowan-Robinson, M., Schulz, B., Scott, Douglas, Seymour, N., Shupe, D. L., Smith, A. J., Symeonidis, M., Valtchanov, I., Viero, M., Wang, L., Wardlow, J., Xu, C. K., Zemcov, M., Marchetti, L., Vaccari, M., Franceschini, A., Arumugam, V., Aussel, H., Bethermin, M., Bock, J., Boselli, A., Buat, V., Burgarella, D., Clements, D. L., Conley, A., Conversi, L., Cooray, A., Dowell, C. D., Farrah, D., Feltre, A., Glenn, J., Griffin, M., Hatziminaoglou, E., Heinis, S., Ibar, E., Ivison, R. J., Nguyen, H. T., O'Halloran, B., Oliver, S. J., Omont, A., Page, M. J., Papageorgiou, A., Pearson, C. P., Perez-Fournon, I., Pohlen, M., Rigopoulou, D., Roseboom, I. G., Rowan-Robinson, M., Schulz, B., Scott, Douglas, Seymour, N., Shupe, D. L., Smith, A. J., Symeonidis, M., Valtchanov, I., Viero, M., Wang, L., Wardlow, J., Xu, C. K., and Zemcov, M.

Abstract

We used wide area surveys over 39 deg$^2$ by the HerMES collaboration, performed with the Herschel Observatory SPIRE multi-wavelength camera, to estimate the low-redshift, $0.02

Published
2015
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35. The Phase Space of z~1.2 SpARCS Clusters: Using Herschel to probe Dust Temperature as a Function of Environment and Accretion History

Author

Noble, A. G., Webb, T. M. A., Yee, H. K. C., Muzzin, A., Wilson, G., van der Burg, R. F. J., Balogh, M. L., Shupe, D. L., Noble, A. G., Webb, T. M. A., Yee, H. K. C., Muzzin, A., Wilson, G., van der Burg, R. F. J., Balogh, M. L., and Shupe, D. L.

Abstract

We present a five-band Herschel study (100-500um) of three galaxy clusters at z~1.2 from the Spitzer Adaptation of the Red-Sequence Cluster Survey (SpARCS). With a sample of 120 spectroscopically-confirmed cluster members, we investigate the role of environment on galaxy properties utilizing the projected cluster phase space (line-of-sight velocity versus clustercentric radius), which probes the time-averaged galaxy density to which a galaxy has been exposed. We divide cluster galaxies into phase-space bins of (r/r200) x (v/sigma_v), tracing a sequence of accretion histories in phase space. Stacking optically star-forming cluster members on the Herschel maps, we measure average infrared star formation rates, and, for the first time in high-redshift galaxy clusters, dust temperatures for dynamically distinct galaxy populations---namely, recent infalls and those that were accreted onto the cluster at an earlier epoch. Proceeding from the infalling to virialized (central) regions of phase space, we find a steady decrease in the specific star formation rate and increase in the stellar age of star-forming cluster galaxies. We perform a probability analysis to investigate all acceptable infrared spectral energy distributions within the full parameter space and measure a ~4 sigma drop in the average dust temperature of cluster galaxies in an intermediate phase-space bin, compared to an otherwise flat trend with phase space. We suggest one plausible quenching mechanism which may be consistent with these trends, invoking ram-pressure stripping of the warmer dust for galaxies within this intermediate accretion phase., Comment: 14 pages, 7 figures, 2 tables; accepted for publication in ApJ

Published
2015
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36. HerMES: candidate high-redshift galaxies discovered with Herschel/SPIRE

Author

Dowell, C. D., Conley, A., Glenn, J., Arumugam, V., Asboth, V., Aussel, H., Bertoldi, F., Bethermin, M., Bock, J., Boselli, A., Bridge, C. R., Buat, V., Burgarella, D., Cabrera-Lavers, A., Casey, C. M., Chapman, S. C., Clements, D. L., Conversi, L., Cooray, A., Dannerbauer, H., De Bernardis, F., Ellsworth-Bowers, T. P., Farrah, D., Franceschini, A., Griffin, M., Gurwell, M. A., Halpern, M., Hatziminaoglou, E., Heinis, S., Ibar, E., Ivison, R. J., Laporte, N., Marchetti, L., Martinez-Navajas, P., Marsden, G., Morrison, G. E., Nguyen, H. T., O'Halloran, B., Oliver, S. J., Omont, A., Page, M. J., Papageorgiou, A., Pearson, C. P., Petitpas, G., Perez-Fournon, I., Pohlen, M., Riechers, D. A., Rigopoulou, D., Roseboom, I. G., Rowan-Robinson, M., Sayers, J., Schulz, B., Scott, D., Seymour, N., Shupe, D. L., Smith, A. J., Streblyanska, A., Symeonidis, M., Vaccari, M., Valtchanov, I., Vieira, J. D., Viero, M., Wang, L., Wardlow, J., Xu, C. K., Zemcov, M., Dowell, C. D., Conley, A., Glenn, J., Arumugam, V., Asboth, V., Aussel, H., Bertoldi, F., Bethermin, M., Bock, J., Boselli, A., Bridge, C. R., Buat, V., Burgarella, D., Cabrera-Lavers, A., Casey, C. M., Chapman, S. C., Clements, D. L., Conversi, L., Cooray, A., Dannerbauer, H., De Bernardis, F., Ellsworth-Bowers, T. P., Farrah, D., Franceschini, A., Griffin, M., Gurwell, M. A., Halpern, M., Hatziminaoglou, E., Heinis, S., Ibar, E., Ivison, R. J., Laporte, N., Marchetti, L., Martinez-Navajas, P., Marsden, G., Morrison, G. E., Nguyen, H. T., O'Halloran, B., Oliver, S. J., Omont, A., Page, M. J., Papageorgiou, A., Pearson, C. P., Petitpas, G., Perez-Fournon, I., Pohlen, M., Riechers, D. A., Rigopoulou, D., Roseboom, I. G., Rowan-Robinson, M., Sayers, J., Schulz, B., Scott, D., Seymour, N., Shupe, D. L., Smith, A. J., Streblyanska, A., Symeonidis, M., Vaccari, M., Valtchanov, I., Vieira, J. D., Viero, M., Wang, L., Wardlow, J., Xu, C. K., and Zemcov, M.

Abstract

We present a method for selecting z > 4 dusty, star-forming galaxies (DSFGs) using Herschel/Spectral and Photometric Imaging Receiver 250/350/500 mu m flux densities to search for red sources. We apply this method to 21 deg(2) of data from the HerMES survey to produce a catalog of 38 high-z candidates. Follow-up of the first five of these sources confirms that this method is efficient at selecting high-z DSFGs, with 4/5 at z = 4.3-6.3 (and the remaining source at z = 3.4), and that they are some of the most luminous dusty sources known. Comparison with previous DSFG samples, mostly selected at longer wavelengths (e. g., 850 mu m) and in single-band surveys, shows that our method is much more efficient at selecting high-z DSFGs, in the sense that a much larger fraction are at z > 3. Correcting for the selection completeness and purity, we find that the number of bright (S-500 (mu m) >= 30 mJy), red Herschel sources is 3.3 +/- 0.8 deg(-2). This is much higher than the number predicted by current models, suggesting that the DSFG population extends to higher redshifts than previously believed. If the shape of the luminosity function for high-z DSFGs is similar to that at z similar to 2, rest-frame UV based studies may be missing a significant component of the star formation density at z = 4-6, even after correction for extinction.

Published
2014
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37. HerMES: candidate high-redshift galaxies discovered with Herschel/SPIRE

Author

Physics, Dowell, C. D., Conley, A., Glenn, J., Arumugam, V., Asboth, V., Aussel, H., Bertoldi, F., Bethermin, M., Bock, J., Boselli, A., Bridge, C. R., Buat, V., Burgarella, D., Cabrera-Lavers, A., Casey, C. M., Chapman, S. C., Clements, D. L., Conversi, L., Cooray, A., Dannerbauer, H., De Bernardis, F., Ellsworth-Bowers, T. P., Farrah, D., Franceschini, A., Griffin, M., Gurwell, M. A., Halpern, M., Hatziminaoglou, E., Heinis, S., Ibar, E., Ivison, R. J., Laporte, N., Marchetti, L., Martinez-Navajas, P., Marsden, G., Morrison, G. E., Nguyen, H. T., O'Halloran, B., Oliver, S. J., Omont, A., Page, M. J., Papageorgiou, A., Pearson, C. P., Petitpas, G., Perez-Fournon, I., Pohlen, M., Riechers, D. A., Rigopoulou, D., Roseboom, I. G., Rowan-Robinson, M., Sayers, J., Schulz, B., Scott, D., Seymour, N., Shupe, D. L., Smith, A. J., Streblyanska, A., Symeonidis, M., Vaccari, M., Valtchanov, I., Vieira, J. D., Viero, M., Wang, L., Wardlow, J., Xu, C. K., Zemcov, M., Physics, Dowell, C. D., Conley, A., Glenn, J., Arumugam, V., Asboth, V., Aussel, H., Bertoldi, F., Bethermin, M., Bock, J., Boselli, A., Bridge, C. R., Buat, V., Burgarella, D., Cabrera-Lavers, A., Casey, C. M., Chapman, S. C., Clements, D. L., Conversi, L., Cooray, A., Dannerbauer, H., De Bernardis, F., Ellsworth-Bowers, T. P., Farrah, D., Franceschini, A., Griffin, M., Gurwell, M. A., Halpern, M., Hatziminaoglou, E., Heinis, S., Ibar, E., Ivison, R. J., Laporte, N., Marchetti, L., Martinez-Navajas, P., Marsden, G., Morrison, G. E., Nguyen, H. T., O'Halloran, B., Oliver, S. J., Omont, A., Page, M. J., Papageorgiou, A., Pearson, C. P., Petitpas, G., Perez-Fournon, I., Pohlen, M., Riechers, D. A., Rigopoulou, D., Roseboom, I. G., Rowan-Robinson, M., Sayers, J., Schulz, B., Scott, D., Seymour, N., Shupe, D. L., Smith, A. J., Streblyanska, A., Symeonidis, M., Vaccari, M., Valtchanov, I., Vieira, J. D., Viero, M., Wang, L., Wardlow, J., Xu, C. K., and Zemcov, M.

Abstract

We present a method for selecting z > 4 dusty, star-forming galaxies (DSFGs) using Herschel/Spectral and Photometric Imaging Receiver 250/350/500 mu m flux densities to search for red sources. We apply this method to 21 deg(2) of data from the HerMES survey to produce a catalog of 38 high-z candidates. Follow-up of the first five of these sources confirms that this method is efficient at selecting high-z DSFGs, with 4/5 at z = 4.3-6.3 (and the remaining source at z = 3.4), and that they are some of the most luminous dusty sources known. Comparison with previous DSFG samples, mostly selected at longer wavelengths (e. g., 850 mu m) and in single-band surveys, shows that our method is much more efficient at selecting high-z DSFGs, in the sense that a much larger fraction are at z > 3. Correcting for the selection completeness and purity, we find that the number of bright (S-500 (mu m) >= 30 mJy), red Herschel sources is 3.3 +/- 0.8 deg(-2). This is much higher than the number predicted by current models, suggesting that the DSFG population extends to higher redshifts than previously believed. If the shape of the luminosity function for high-z DSFGs is similar to that at z similar to 2, rest-frame UV based studies may be missing a significant component of the star formation density at z = 4-6, even after correction for extinction.

Published
2014

38. The suppression of star formation by powerful active galactic nuclei

Author

Page, M. J., Symeonidis, M., Vieira, J. D., Altieri, B., Amblard, A., Arumugam, V., Aussel, H., Babbedge, T., Blain, A., Bock, J., Boselli, A., Buat, V., Castro-Rodr'iguez, N., Cava, A., Chanial, P., Clements, D. L., Conley, A., Conversi, L., Cooray, A., Dowell, C. D., Dubois, E. N., Dunlop, J. S., Dwek, E., Dye, S., Eales, S., Elbaz, D., Farrah, D., Fox, M., Franceschini, A., Gear, W., Glenn, J., Griffin, M., Halpern, M., Hatziminaoglou, E., Ibar, E., Isaak, K., Ivison, R. J., Lagache, G., Levenson, L., Lu, N., Madden, S., Maffei, B., Mainetti, G., Marchetti, L., Nguyen, H. T., O'Halloran, B., Oliver, S. J., Omont, A., Panuzzo, P., Papageorgiou, A., Pearson, C. P., Perez-Fournon, I., Pohlen, M., Rawlings, J. I., Rigopoulou, D., Riguccini, L., Rizzo, D., Rodighiero, G., Roseboom, I. G., Rowan-Robinson, M., Portal, M. Sanchez, Schulz, B., Scott, Douglas, Seymour, N., Shupe, D. L., Smith, A. J., Stevens, J. A., Trichas, M., Tugwell, K. E., Vaccari, M., Valtchanov, I., Viero, M., Vigroux, L., Wang, L., Ward, R., Wright, G., Xu, C. K., Zemcov, M., Page, M. J., Symeonidis, M., Vieira, J. D., Altieri, B., Amblard, A., Arumugam, V., Aussel, H., Babbedge, T., Blain, A., Bock, J., Boselli, A., Buat, V., Castro-Rodr'iguez, N., Cava, A., Chanial, P., Clements, D. L., Conley, A., Conversi, L., Cooray, A., Dowell, C. D., Dubois, E. N., Dunlop, J. S., Dwek, E., Dye, S., Eales, S., Elbaz, D., Farrah, D., Fox, M., Franceschini, A., Gear, W., Glenn, J., Griffin, M., Halpern, M., Hatziminaoglou, E., Ibar, E., Isaak, K., Ivison, R. J., Lagache, G., Levenson, L., Lu, N., Madden, S., Maffei, B., Mainetti, G., Marchetti, L., Nguyen, H. T., O'Halloran, B., Oliver, S. J., Omont, A., Panuzzo, P., Papageorgiou, A., Pearson, C. P., Perez-Fournon, I., Pohlen, M., Rawlings, J. I., Rigopoulou, D., Riguccini, L., Rizzo, D., Rodighiero, G., Roseboom, I. G., Rowan-Robinson, M., Portal, M. Sanchez, Schulz, B., Scott, Douglas, Seymour, N., Shupe, D. L., Smith, A. J., Stevens, J. A., Trichas, M., Tugwell, K. E., Vaccari, M., Valtchanov, I., Viero, M., Vigroux, L., Wang, L., Ward, R., Wright, G., Xu, C. K., and Zemcov, M.

Abstract

The old, red stars which constitute the bulges of galaxies, and the massive black holes at their centres, are the relics of a period in cosmic history when galaxies formed stars at remarkable rates and active galactic nuclei (AGN) shone brightly from accretion onto black holes. It is widely suspected, but unproven, that the tight correlation in mass of the black hole and stellar components results from the AGN quenching the surrounding star formation as it approaches its peak luminosity. X-rays trace emission from AGN unambiguously, while powerful star-forming galaxies are usually dust-obscured and are brightest at infrared to submillimetre wavelengths. Here we report observations in the submillimetre and X-ray which show that rapid star formation was common in the host galaxies of AGN when the Universe was 2-6 Gyrs old, but that the most vigorous star formation is not observed around black holes above an X-ray luminosity of 10^44 erg/s. This suppression of star formation in the host galaxies of powerful AGN is a key prediction of models in which the AGN drives a powerful outflow, expelling the interstellar medium of its host galaxy and transforming the galaxy's properties in a brief period of cosmic time., Comment: Published in Nature, May 2012. Includes supplementary information

Published
2013
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39. HerMES: Candidate High-Redshift Galaxies Discovered with Herschel/SPIRE

Author

Dowell, C. Darren, Conley, A., Glenn, J., Arumugam, V., Asboth, V., Aussel, H., Bertoldi, F., Bethermin, M., Bock, J., Boselli, A., Bridge, C., Buat, V., Burgarella, D., Cabrera-Lavers, A., Casey, C. M., Chapman, S. C., Clements, D. L., Conversi, L., Cooray, A., Dannerbauer, H., De Bernardis, F., Ellsworth-Bowers, T. P., Farrah, D., Franceschini, A., Griffin, M., Gurwell, M. A., Halpern, M., Hatziminaoglou, E., Heinis, S., Ibar, E., Ivison, R. J., Laporte, N., Marchetti, L., Martinez-Navajas, P., Marsden, G., Morrison, G. E., Nguyen, H. T., O'Halloran, B., Oliver, S. J., Omont, A., Page, M. J., Papageorgiou, A., Pearson, C. P., Petitpas, G., Perez-Fournon, I., Pohlen, M., Riechers, D., Rigopoulou, D., Roseboom, I. G., Rowan-Robinson, M., Sayers, J., Schulz, B., Scott, Douglas, Seymour, N., Shupe, D. L., Smith, A. J., Streblyanska, A., Symeonidis, M., Vaccari, M., Valtchanov, I., Vieira, J. D., Viero, M., Wang, L., Wardlow, J., Xu, C. K., Zemcov, M., Dowell, C. Darren, Conley, A., Glenn, J., Arumugam, V., Asboth, V., Aussel, H., Bertoldi, F., Bethermin, M., Bock, J., Boselli, A., Bridge, C., Buat, V., Burgarella, D., Cabrera-Lavers, A., Casey, C. M., Chapman, S. C., Clements, D. L., Conversi, L., Cooray, A., Dannerbauer, H., De Bernardis, F., Ellsworth-Bowers, T. P., Farrah, D., Franceschini, A., Griffin, M., Gurwell, M. A., Halpern, M., Hatziminaoglou, E., Heinis, S., Ibar, E., Ivison, R. J., Laporte, N., Marchetti, L., Martinez-Navajas, P., Marsden, G., Morrison, G. E., Nguyen, H. T., O'Halloran, B., Oliver, S. J., Omont, A., Page, M. J., Papageorgiou, A., Pearson, C. P., Petitpas, G., Perez-Fournon, I., Pohlen, M., Riechers, D., Rigopoulou, D., Roseboom, I. G., Rowan-Robinson, M., Sayers, J., Schulz, B., Scott, Douglas, Seymour, N., Shupe, D. L., Smith, A. J., Streblyanska, A., Symeonidis, M., Vaccari, M., Valtchanov, I., Vieira, J. D., Viero, M., Wang, L., Wardlow, J., Xu, C. K., and Zemcov, M.

Abstract

We present a method for selecting $z>4$ dusty, star forming galaxies (DSFGs) using Herschel/SPIRE 250/350/500 $\mu m$ flux densities to search for red sources. We apply this method to 21 deg$^2$ of data from the HerMES survey to produce a catalog of 38 high-$z$ candidates. Follow-up of the first 5 of these sources confirms that this method is efficient at selecting high-$z$ DSFGs, with 4/5 at $z=4.3$ to $6.3$ (and the remaining source at $z=3.4$), and that they are some of the most luminous dusty sources known. Comparison with previous DSFG samples, mostly selected at longer wavelengths (e.g., 850 $\mu m$) and in single-band surveys, shows that our method is much more efficient at selecting high-$z$ DSFGs, in the sense that a much larger fraction are at $z>3$. Correcting for the selection completeness and purity, we find that the number of bright ($S_{500\,\mu m} \ge 30$ mJy), red Herschel sources is $3.3 \pm 0.8$ deg$^{-2}$. This is much higher than the number predicted by current models, suggesting that the DSFG population extends to higher redshifts than previously believed. If the shape of the luminosity function for high-$z$ DSFGs is similar to that at $z\sim2$, rest-frame UV based studies may be missing a significant component of the star formation density at $z=4$ to $6$, even after correction for extinction., Comment: Accepted for publication in ApJ

Published
2013
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40. Flux calibration of the Herschel-SPIRE photometer

Author

Bendo, G. J., Griffin, M. J., Bock, J. J., Conversi, L., Dowell, C. D., Lim, T., Lu, N., North, C. E., Papageorgiou, A., Pearson, C. P., Pohlen, M., Polehampton, E. T., Schulz, B., Shupe, D. L., Sibthorpe, B., Spencer, L. D., Swinyard, B. M., Valtchanov, I., Xu, C. K., Bendo, G. J., Griffin, M. J., Bock, J. J., Conversi, L., Dowell, C. D., Lim, T., Lu, N., North, C. E., Papageorgiou, A., Pearson, C. P., Pohlen, M., Polehampton, E. T., Schulz, B., Shupe, D. L., Sibthorpe, B., Spencer, L. D., Swinyard, B. M., Valtchanov, I., and Xu, C. K.

Abstract

We describe the procedure used to flux calibrate the three-band submillimetre photometer in the Spectral and Photometric Imaging REceiver (SPIRE) instrument on the Herschel Space Observatory. This includes the equations describing the calibration scheme, a justification for using Neptune as the primary calibration source, a description of the observations and data processing procedures used to derive flux calibration parameters (for converting from voltage to flux density) for every bolometer in each array, an analysis of the error budget in the flux calibration for the individual bolometers, and tests of the flux calibration on observations of primary and secondary calibrators. The procedure for deriving the flux calibration parameters is divided into two parts. In the first part, we use observations of astronomical sources in conjunction with the operation of the photometer internal calibration source to derive the unscaled derivatives of the flux calibration curves. To scale the calibration curves in Jy/beam/V, we then use observations of Neptune in which the beam of each bolometer is mapped using Neptune observed in a very fine scan pattern. The total instrumental uncertainties in the flux calibration for the individual bolometers is ~0.5% for most bolometers, although a few bolometers have uncertainties of ~1-5% because of issues with the Neptune observations. Based on application of the flux calibration parameters to Neptune observations performed using typical scan map observing modes, we determined that measurements from each array as a whole have instrumental uncertainties of 1.5%. This is considerably less than the absolute calibration uncertainty associated with the model of Neptune, which is estimated at 4%., Comment: 20 pages, 17 figures, accepted for publication in MNRAS

Published
2013
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41. HerMES: A Deficit in the Surface Brightness of the Cosmic Infrared Background Due to Galaxy Cluster Gravitational Lensing

Author

Zemcov, M., Blain, A., Cooray, A., Bethermin, M., Bock, J., Clements, D. L., Conley, A., Conversi, L., Dowell, C. D., Farrah, D., Glenn, J., Griffin, M., Halpern, M., Jullo, E., Kneib, J. -P., Marsden, G., Nguyen, H. T., Richard, S. J. Oliver J., Roseboom, I. G., Schulz, B., Scott, Douglas, Shupe, D. L., Smith, A. J., Valtchanov, I., Viero, M., Wang, L., Wardlow, J., Zemcov, M., Blain, A., Cooray, A., Bethermin, M., Bock, J., Clements, D. L., Conley, A., Conversi, L., Dowell, C. D., Farrah, D., Glenn, J., Griffin, M., Halpern, M., Jullo, E., Kneib, J. -P., Marsden, G., Nguyen, H. T., Richard, S. J. Oliver J., Roseboom, I. G., Schulz, B., Scott, Douglas, Shupe, D. L., Smith, A. J., Valtchanov, I., Viero, M., Wang, L., and Wardlow, J.

Abstract

We have observed four massive galaxy clusters with the SPIRE instrument on the Herschel Space Observatory and measure a deficit of surface brightness within their central region after subtracting sources. We simulate the effects of instrumental sensitivity and resolution, the source population, and the lensing effect of the clusters to estimate the shape and amplitude of the deficit. The amplitude of the central deficit is a strong function of the surface density and flux distribution of the background sources. We find that for the current best fitting faint end number counts, and excellent lensing models, the most likely amplitude of the central deficit is the full intensity of the cosmic infrared background (CIB). Our measurement leads to a lower limit to the integrated total intensity of the CIB of I(250 microns) > 0.69_(-0.03)^(+0.03) (stat.)_(-0.06)^(+0.11) (sys.) MJy/sr, with more CIB possible from both low-redshift sources and from sources within the target clusters. It should be possible to observe this effect in existing high angular resolution data at other wavelengths where the CIB is bright, which would allow tests of models of the faint source component of the CIB., Comment: 5 pages, 3 figures, replacing with version matching published manuscript

Published
2013
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42. The Herschel PEP/HerMES Luminosity Function. I: Probing the Evolution of PACS selected Galaxies to z~4

Author

Gruppioni, C., Pozzi, F., Rodighiero, G., Delvecchio, I., Berta, S., Pozzetti, L., Zamorani, G., Andreani, P., Cimatti, A., Ilbert, O., Floch, E. Le, Lutz, D., Magnelli, B., Marchetti, L., Monaco, P., Nordon, R., Oliver, S., Popesso, P., Riguccini, L., Roseboom, I., Rosario, D. J., Sargent, M., Vaccari, M., Altieri, B., Aussel, H., Bongiovanni, A., Cepa, J., Daddi, E., Dominguez-Sanchez, H., Elbaz, D., Forster-Schreiber, N., Genzel, R., Iribarrem, A., Magliocchetti, M., Maiolino, R., Poglitsch, A., Garcia, A. Perez, Sanchez-Portal, M., Sturm, E., Tacconi, L., Valtchanov, I., Amblard, A., Arumugam, V., Bethermin, M., Bock, J., Boselli, A., Buat, V., Burgarella, D., Castro-Rodriguez, N., Cava, A., Chanial, P., Clements, D. L., Conley, A., Cooray, A., Dowell, C. D., Dwek, E., Eales, S., Franceschini, A., Glenn, J., Griffin, M., Hatziminaoglou, E., Ibar, E., Isaak, K., Ivison, R. J., Lagache, G., Levenson, L., Lu, N., Madden, S., Maffei, B., Mainetti, G., Nguyen, H. T., Halloran, B. O, Page, M. J., Panuzzo, P., Papageorgiou, A., Pearson, C. P., Perez-Fournon, I., Pohlen, M., Rigopoulou, D., Rowan-Robinson, M., Schulz, B., Scott, D., Seymour, N., Shupe, D. L., Smith, A. J., Stevens, J. A., Symeonidis, M., Trichas, M., Tugwell, K. E., Vigroux, L., Wang, L., Wright, G., Xu, C. K., Zemcov, M., Bardelli, S., Carollo, M., Contini, T., Fevre, O. Le, Lilly, S., Mainieri, V., Renzini, A., Scodeggio, M., Zucca, E., Gruppioni, C., Pozzi, F., Rodighiero, G., Delvecchio, I., Berta, S., Pozzetti, L., Zamorani, G., Andreani, P., Cimatti, A., Ilbert, O., Floch, E. Le, Lutz, D., Magnelli, B., Marchetti, L., Monaco, P., Nordon, R., Oliver, S., Popesso, P., Riguccini, L., Roseboom, I., Rosario, D. J., Sargent, M., Vaccari, M., Altieri, B., Aussel, H., Bongiovanni, A., Cepa, J., Daddi, E., Dominguez-Sanchez, H., Elbaz, D., Forster-Schreiber, N., Genzel, R., Iribarrem, A., Magliocchetti, M., Maiolino, R., Poglitsch, A., Garcia, A. Perez, Sanchez-Portal, M., Sturm, E., Tacconi, L., Valtchanov, I., Amblard, A., Arumugam, V., Bethermin, M., Bock, J., Boselli, A., Buat, V., Burgarella, D., Castro-Rodriguez, N., Cava, A., Chanial, P., Clements, D. L., Conley, A., Cooray, A., Dowell, C. D., Dwek, E., Eales, S., Franceschini, A., Glenn, J., Griffin, M., Hatziminaoglou, E., Ibar, E., Isaak, K., Ivison, R. J., Lagache, G., Levenson, L., Lu, N., Madden, S., Maffei, B., Mainetti, G., Nguyen, H. T., Halloran, B. O, Page, M. J., Panuzzo, P., Papageorgiou, A., Pearson, C. P., Perez-Fournon, I., Pohlen, M., Rigopoulou, D., Rowan-Robinson, M., Schulz, B., Scott, D., Seymour, N., Shupe, D. L., Smith, A. J., Stevens, J. A., Symeonidis, M., Trichas, M., Tugwell, K. E., Vigroux, L., Wang, L., Wright, G., Xu, C. K., Zemcov, M., Bardelli, S., Carollo, M., Contini, T., Fevre, O. Le, Lilly, S., Mainieri, V., Renzini, A., Scodeggio, M., and Zucca, E.

Abstract

We exploit the deep and extended far infrared data sets (at 70, 100 and 160 um) of the Herschel GTO PACS Evolutionary Probe (PEP) Survey, in combination with the HERschel Multi tiered Extragalactic Survey (HerMES) data at 250, 350 and 500 um, to derive the evolution of the restframe 35 um, 60 um, 90 um, and total infrared (IR) luminosity functions (LFs) up to z~4. We detect very strong luminosity evolution for the total IR LF combined with a density evolution. In agreement with previous findings, the IR luminosity density increases steeply to z~1, then flattens between z~1 and z~3 to decrease at z greater than 3. Galaxies with different SEDs, masses and sSFRs evolve in very different ways and this large and deep statistical sample is the first one allowing us to separately study the different evolutionary behaviours of the individual IR populations contributing to the IR luminosity density. Galaxies occupying the well established SFR/stellar mass main sequence (MS) are found to dominate both the total IR LF and luminosity density at all redshifts, with the contribution from off MS sources (0.6 dex above MS) being nearly constant (~20% of the total IR luminosity density) and showing no significant signs of increase with increasing z over the whole 0.8

Published
2013
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43. The Herschel census of infrared SEDs through cosmic time

Author

Symeonidis, Myrto, Vaccari, M., Berta, S., Page, M. J., Lutz, D., Arumugam, V., Aussel, H., Bock, J., Boselli, A., Buat, V., Capak, P. L., Clements, D. L., Conley, A., Conversi, L., Cooray, A., Dowell, C. D., Farrah, D., Franceschini, A., Giovannoli, E., Glenn, J., Griffin, M., Hatziminaoglou, E., Hwang, H. -S., Ibar, E., Ilbert, O., Ivison, R. J., Floc'h, E. Le, Lilly, S., Kartaltepe, J. S., Magnelli, B., Magdis, G., Marchetti, L., Nguyen, H. T., Nordon, R., O'Halloran, B., Oliver, S. J., Omont, A., Papageorgiou, A., Patel, H., Pearson, C. P., Perez-Fournon, I., Pohlen, M., Popesso, P., Pozzi, F., Rigopoulou, D., Riguccini, L., Rosario, D., Roseboom, I. G., Rowan-Robinson, M., Salvato, M., Schulz, B., Scott, Douglas, Seymour, N., Shupe, D. L., Smith, A. J., Valtchanov, I., Wang, L., Xu, C. K., Zemcov, M., Wuyts, S., Symeonidis, Myrto, Vaccari, M., Berta, S., Page, M. J., Lutz, D., Arumugam, V., Aussel, H., Bock, J., Boselli, A., Buat, V., Capak, P. L., Clements, D. L., Conley, A., Conversi, L., Cooray, A., Dowell, C. D., Farrah, D., Franceschini, A., Giovannoli, E., Glenn, J., Griffin, M., Hatziminaoglou, E., Hwang, H. -S., Ibar, E., Ilbert, O., Ivison, R. J., Floc'h, E. Le, Lilly, S., Kartaltepe, J. S., Magnelli, B., Magdis, G., Marchetti, L., Nguyen, H. T., Nordon, R., O'Halloran, B., Oliver, S. J., Omont, A., Papageorgiou, A., Patel, H., Pearson, C. P., Perez-Fournon, I., Pohlen, M., Popesso, P., Pozzi, F., Rigopoulou, D., Riguccini, L., Rosario, D., Roseboom, I. G., Rowan-Robinson, M., Salvato, M., Schulz, B., Scott, Douglas, Seymour, N., Shupe, D. L., Smith, A. J., Valtchanov, I., Wang, L., Xu, C. K., Zemcov, M., and Wuyts, S.

Abstract

Using Herschel data from the deepest SPIRE and PACS surveys (HerMES and PEP) in COSMOS and GOODS (N+S), we examine the dust properties of IR-luminous (L_IR>10^10 L_sun) galaxies at 0.145K) SEDs and cold (T<25K), cirrus-dominated SEDs are rare, with most sources being within the range occupied by warm starbursts such as M82 and cool spirals such as M51. We observe a luminosity-temperature (L-T) relation, where the average dust temperature of log[L_IR/L_sun]=12.5 galaxies is about 10K higher than that of their log[L_IR/L_sun]=10.5 counterparts. However, although the increased dust heating in more luminous systems is the driving factor behind the L-T relation, the increase in dust mass and/or starburst size with luminosity plays a dominant role in shaping it. Our results show that the dust conditions in IR-luminous sources evolve with cosmic time: at high redshift, dust temperatures are on average up to 10K lower than what is measured locally. This is manifested as a flattening of the L-T relation, suggesting that (U)LIRGs in the early Universe are typically characterised by a more extended dust distribution and/or higher dust masses than local equivalent sources. Interestingly, the evolution in dust temperature is luminosity dependent, with the fraction of LIRGs with T<35K showing a 2-fold increase from z~0 to z~2, whereas that of ULIRGs with T<35K shows a 6-fold increase., Comment: 27 pages, 23 figures, 2 tables, accepted for publication in MNRAS

Published
2013
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44. HerMES: a deficit in the surface brightness of the cosmic infrared background due to galaxy cluster gravitational lensing

Author

Zemcov, M., Blain, A., Cooray, A., Bethermin, M., Bock, J., Clements, D. L., Conley, A., Conversi, L., Dowell, C. D., Farrah, D., Glenn, J., Griffin, M., Halpern, M., Jullo, E., Kneib, J. P., Marsden, G., Nguyen, H. T., Oliver, S. J., Richard, J., Roseboom, I. G., Schulz, B., Scott, D., Shupe, D. L., Smith, A. J., Valtchanov, I., Viero, M., Wang, L., Wardlow, J., Zemcov, M., Blain, A., Cooray, A., Bethermin, M., Bock, J., Clements, D. L., Conley, A., Conversi, L., Dowell, C. D., Farrah, D., Glenn, J., Griffin, M., Halpern, M., Jullo, E., Kneib, J. P., Marsden, G., Nguyen, H. T., Oliver, S. J., Richard, J., Roseboom, I. G., Schulz, B., Scott, D., Shupe, D. L., Smith, A. J., Valtchanov, I., Viero, M., Wang, L., and Wardlow, J.

Abstract

We have observed four massive galaxy clusters with the SPIRE instrument on the Herschel Space Observatory and measure a deficit of surface brightness within their central region after removing detected sources. We simulate the effects of instrumental sensitivity and resolution, the source population, and the lensing effect of the clusters to estimate the shape and amplitude of the deficit. The amplitude of the central deficit is a strong function of the surface density and flux distribution of the background sources. We find that for the current best fitting faint end number counts, and excellent lensing models, the most likely amplitude of the central deficit is the full intensity of the cosmic infrared background (CIB). Our measurement leads to a lower limit to the integrated total intensity of the CIB of I-250 mu m > 0.69(-0.03)(+0.03)(stat.)(-0.06)(+0.11)(sys.) MJy sr(-1), with more CIB possible from both low-redshift sources and from sources within the target clusters. It should be possible to observe this effect in existing high angular resolution data at other wavelengths where the CIB is bright, which would allow tests of models of the faint source component of the CIB.

Published
2013
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45. HerMES: A Deficit in the Surface Brightness of the Cosmic Infrared Background due to Galaxy Cluster Gravitational Lensing

Author

Zemcov, M., Blain, A., Cooray, A., Béthermin, M., Bock, J., Clements, D. L., Conley, A., Conversi, L., Dowell, C. D., Farrah, D., Glenn, J., Griffin, M., Halpern, M., Jullo, E., Kneib, J.-P., Marsden, G., Nguyen, H. T., Oliver, S. J., Richard, J., Roseboom, I. G., Schulz, B., Scott, Douglas, Shupe, D. L., Smith, A. J., Valtchanov, I., Viero, M., Wang, L., Wardlow, J., Zemcov, M., Blain, A., Cooray, A., Béthermin, M., Bock, J., Clements, D. L., Conley, A., Conversi, L., Dowell, C. D., Farrah, D., Glenn, J., Griffin, M., Halpern, M., Jullo, E., Kneib, J.-P., Marsden, G., Nguyen, H. T., Oliver, S. J., Richard, J., Roseboom, I. G., Schulz, B., Scott, Douglas, Shupe, D. L., Smith, A. J., Valtchanov, I., Viero, M., Wang, L., and Wardlow, J.

Abstract

We have observed four massive galaxy clusters with the SPIRE instrument on the Herschel Space Observatory and measure a deficit of surface brightness within their central region after removing detected sources. We simulate the effects of instrumental sensitivity and resolution, the source population, and the lensing effect of the clusters to estimate the shape and amplitude of the deficit. The amplitude of the central deficit is a strong function of the surface density and flux distribution of the background sources. We find that for the current best fitting faint end number counts, and excellent lensing models, the most likely amplitude of the central deficit is the full intensity of the cosmic infrared background (CIB). Our measurement leads to a lower limit to the integrated total intensity of the CIB of I_{250 \, \mu {m}} \gt 0.69_{-0.03}^{+0.03} ({stat.}) _{-0.06}^{+0.11} ({sys.}) MJy sr-1, with more CIB possible from both low-redshift sources and from sources within the target clusters. It should be possible to observe this effect in existing high angular resolution data at other wavelengths where the CIB is bright, which would allow tests of models of the faint source component of the CIB. Herschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA.

Published
2013

46. HerMES: A Deficit in the Surface Brightness of the Cosmic Infrared Background due to Galaxy Cluster Gravitational Lensing

Author

Zemcov, M., Blain, A., Cooray, A., Béthermin, M., Bock, J., Clements, D. L., Conley, A., Conversi, L., Dowell, C. D., Farrah, D., Glenn, J., Griffin, M., Halpern, M., Jullo, E., Kneib, J.-P., Marsden, G., Nguyen, H. T., Oliver, S. J., Richard, J., Roseboom, I. G., Schulz, B., Scott, Douglas, Shupe, D. L., Smith, A. J., Valtchanov, I., Viero, M., Wang, L., Wardlow, J., Zemcov, M., Blain, A., Cooray, A., Béthermin, M., Bock, J., Clements, D. L., Conley, A., Conversi, L., Dowell, C. D., Farrah, D., Glenn, J., Griffin, M., Halpern, M., Jullo, E., Kneib, J.-P., Marsden, G., Nguyen, H. T., Oliver, S. J., Richard, J., Roseboom, I. G., Schulz, B., Scott, Douglas, Shupe, D. L., Smith, A. J., Valtchanov, I., Viero, M., Wang, L., and Wardlow, J.

Abstract

We have observed four massive galaxy clusters with the SPIRE instrument on the Herschel Space Observatory and measure a deficit of surface brightness within their central region after removing detected sources. We simulate the effects of instrumental sensitivity and resolution, the source population, and the lensing effect of the clusters to estimate the shape and amplitude of the deficit. The amplitude of the central deficit is a strong function of the surface density and flux distribution of the background sources. We find that for the current best fitting faint end number counts, and excellent lensing models, the most likely amplitude of the central deficit is the full intensity of the cosmic infrared background (CIB). Our measurement leads to a lower limit to the integrated total intensity of the CIB of I_{250 \, \mu {m}} \gt 0.69_{-0.03}^{+0.03} ({stat.}) _{-0.06}^{+0.11} ({sys.}) MJy sr-1, with more CIB possible from both low-redshift sources and from sources within the target clusters. It should be possible to observe this effect in existing high angular resolution data at other wavelengths where the CIB is bright, which would allow tests of models of the faint source component of the CIB. Herschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA.

Published
2013

47. HerMES: a deficit in the surface brightness of the cosmic infrared background due to galaxy cluster gravitational lensing

Author

Physics, Zemcov, M., Blain, A., Cooray, A., Bethermin, M., Bock, J., Clements, D. L., Conley, A., Conversi, L., Dowell, C. D., Farrah, D., Glenn, J., Griffin, M., Halpern, M., Jullo, E., Kneib, J. P., Marsden, G., Nguyen, H. T., Oliver, S. J., Richard, J., Roseboom, I. G., Schulz, B., Scott, D., Shupe, D. L., Smith, A. J., Valtchanov, I., Viero, M., Wang, L., Wardlow, J., Physics, Zemcov, M., Blain, A., Cooray, A., Bethermin, M., Bock, J., Clements, D. L., Conley, A., Conversi, L., Dowell, C. D., Farrah, D., Glenn, J., Griffin, M., Halpern, M., Jullo, E., Kneib, J. P., Marsden, G., Nguyen, H. T., Oliver, S. J., Richard, J., Roseboom, I. G., Schulz, B., Scott, D., Shupe, D. L., Smith, A. J., Valtchanov, I., Viero, M., Wang, L., and Wardlow, J.

Abstract

We have observed four massive galaxy clusters with the SPIRE instrument on the Herschel Space Observatory and measure a deficit of surface brightness within their central region after removing detected sources. We simulate the effects of instrumental sensitivity and resolution, the source population, and the lensing effect of the clusters to estimate the shape and amplitude of the deficit. The amplitude of the central deficit is a strong function of the surface density and flux distribution of the background sources. We find that for the current best fitting faint end number counts, and excellent lensing models, the most likely amplitude of the central deficit is the full intensity of the cosmic infrared background (CIB). Our measurement leads to a lower limit to the integrated total intensity of the CIB of I-250 mu m > 0.69(-0.03)(+0.03)(stat.)(-0.06)(+0.11)(sys.) MJy sr(-1), with more CIB possible from both low-redshift sources and from sources within the target clusters. It should be possible to observe this effect in existing high angular resolution data at other wavelengths where the CIB is bright, which would allow tests of models of the faint source component of the CIB.

Published
2013

48. HerMES: Candidate High-Redshift Galaxies Discovered with Herschel/SPIRE

Author

Dowell, C. Darren, Conley, A., Glenn, J., Arumugam, V., Asboth, V., Aussel, H., Bertoldi, F., Bethermin, M., Bock, J., Boselli, A., Bridge, C., Buat, V., Burgarella, D., Cabrera-Lavers, A., Casey, C. M., Chapman, S. C., Clements, D. L., Conversi, L., Cooray, A., Dannerbauer, H., De Bernardis, F., Ellsworth-Bowers, T. P., Farrah, D., Franceschini, A., Griffin, M., Gurwell, M. A., Halpern, M., Hatziminaoglou, E., Heinis, S., Ibar, E., Ivison, R. J., Laporte, N., Marchetti, L., Martinez-Navajas, P., Marsden, G., Morrison, G. E., Nguyen, H. T., O'Halloran, B., Oliver, S. J., Omont, A., Page, M. J., Papageorgiou, A., Pearson, C. P., Petitpas, G., Perez-Fournon, I., Pohlen, M., Riechers, D., Rigopoulou, D., Roseboom, I. G., Rowan-Robinson, M., Sayers, J., Schulz, B., Scott, Douglas, Seymour, N., Shupe, D. L., Smith, A. J., Streblyanska, A., Symeonidis, M., Vaccari, M., Valtchanov, I., Vieira, J. D., Viero, M., Wang, L., Wardlow, J., Xu, C. K., Zemcov, M., Dowell, C. Darren, Conley, A., Glenn, J., Arumugam, V., Asboth, V., Aussel, H., Bertoldi, F., Bethermin, M., Bock, J., Boselli, A., Bridge, C., Buat, V., Burgarella, D., Cabrera-Lavers, A., Casey, C. M., Chapman, S. C., Clements, D. L., Conversi, L., Cooray, A., Dannerbauer, H., De Bernardis, F., Ellsworth-Bowers, T. P., Farrah, D., Franceschini, A., Griffin, M., Gurwell, M. A., Halpern, M., Hatziminaoglou, E., Heinis, S., Ibar, E., Ivison, R. J., Laporte, N., Marchetti, L., Martinez-Navajas, P., Marsden, G., Morrison, G. E., Nguyen, H. T., O'Halloran, B., Oliver, S. J., Omont, A., Page, M. J., Papageorgiou, A., Pearson, C. P., Petitpas, G., Perez-Fournon, I., Pohlen, M., Riechers, D., Rigopoulou, D., Roseboom, I. G., Rowan-Robinson, M., Sayers, J., Schulz, B., Scott, Douglas, Seymour, N., Shupe, D. L., Smith, A. J., Streblyanska, A., Symeonidis, M., Vaccari, M., Valtchanov, I., Vieira, J. D., Viero, M., Wang, L., Wardlow, J., Xu, C. K., and Zemcov, M.

Abstract

We present a method for selecting $z>4$ dusty, star forming galaxies (DSFGs) using Herschel/SPIRE 250/350/500 $\mu m$ flux densities to search for red sources. We apply this method to 21 deg$^2$ of data from the HerMES survey to produce a catalog of 38 high-$z$ candidates. Follow-up of the first 5 of these sources confirms that this method is efficient at selecting high-$z$ DSFGs, with 4/5 at $z=4.3$ to $6.3$ (and the remaining source at $z=3.4$), and that they are some of the most luminous dusty sources known. Comparison with previous DSFG samples, mostly selected at longer wavelengths (e.g., 850 $\mu m$) and in single-band surveys, shows that our method is much more efficient at selecting high-$z$ DSFGs, in the sense that a much larger fraction are at $z>3$. Correcting for the selection completeness and purity, we find that the number of bright ($S_{500\,\mu m} \ge 30$ mJy), red Herschel sources is $3.3 \pm 0.8$ deg$^{-2}$. This is much higher than the number predicted by current models, suggesting that the DSFG population extends to higher redshifts than previously believed. If the shape of the luminosity function for high-$z$ DSFGs is similar to that at $z\sim2$, rest-frame UV based studies may be missing a significant component of the star formation density at $z=4$ to $6$, even after correction for extinction., Comment: Accepted for publication in ApJ

Published
2013
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49. The suppression of star formation by powerful active galactic nuclei

Author

Page, M. J., Symeonidis, M., Vieira, J. D., Altieri, B., Amblard, A., Arumugam, V., Aussel, H., Babbedge, T., Blain, A., Bock, J., Boselli, A., Buat, V., Castro-Rodr'iguez, N., Cava, A., Chanial, P., Clements, D. L., Conley, A., Conversi, L., Cooray, A., Dowell, C. D., Dubois, E. N., Dunlop, J. S., Dwek, E., Dye, S., Eales, S., Elbaz, D., Farrah, D., Fox, M., Franceschini, A., Gear, W., Glenn, J., Griffin, M., Halpern, M., Hatziminaoglou, E., Ibar, E., Isaak, K., Ivison, R. J., Lagache, G., Levenson, L., Lu, N., Madden, S., Maffei, B., Mainetti, G., Marchetti, L., Nguyen, H. T., O'Halloran, B., Oliver, S. J., Omont, A., Panuzzo, P., Papageorgiou, A., Pearson, C. P., Perez-Fournon, I., Pohlen, M., Rawlings, J. I., Rigopoulou, D., Riguccini, L., Rizzo, D., Rodighiero, G., Roseboom, I. G., Rowan-Robinson, M., Portal, M. Sanchez, Schulz, B., Scott, Douglas, Seymour, N., Shupe, D. L., Smith, A. J., Stevens, J. A., Trichas, M., Tugwell, K. E., Vaccari, M., Valtchanov, I., Viero, M., Vigroux, L., Wang, L., Ward, R., Wright, G., Xu, C. K., Zemcov, M., Page, M. J., Symeonidis, M., Vieira, J. D., Altieri, B., Amblard, A., Arumugam, V., Aussel, H., Babbedge, T., Blain, A., Bock, J., Boselli, A., Buat, V., Castro-Rodr'iguez, N., Cava, A., Chanial, P., Clements, D. L., Conley, A., Conversi, L., Cooray, A., Dowell, C. D., Dubois, E. N., Dunlop, J. S., Dwek, E., Dye, S., Eales, S., Elbaz, D., Farrah, D., Fox, M., Franceschini, A., Gear, W., Glenn, J., Griffin, M., Halpern, M., Hatziminaoglou, E., Ibar, E., Isaak, K., Ivison, R. J., Lagache, G., Levenson, L., Lu, N., Madden, S., Maffei, B., Mainetti, G., Marchetti, L., Nguyen, H. T., O'Halloran, B., Oliver, S. J., Omont, A., Panuzzo, P., Papageorgiou, A., Pearson, C. P., Perez-Fournon, I., Pohlen, M., Rawlings, J. I., Rigopoulou, D., Riguccini, L., Rizzo, D., Rodighiero, G., Roseboom, I. G., Rowan-Robinson, M., Portal, M. Sanchez, Schulz, B., Scott, Douglas, Seymour, N., Shupe, D. L., Smith, A. J., Stevens, J. A., Trichas, M., Tugwell, K. E., Vaccari, M., Valtchanov, I., Viero, M., Vigroux, L., Wang, L., Ward, R., Wright, G., Xu, C. K., and Zemcov, M.

Abstract

The old, red stars which constitute the bulges of galaxies, and the massive black holes at their centres, are the relics of a period in cosmic history when galaxies formed stars at remarkable rates and active galactic nuclei (AGN) shone brightly from accretion onto black holes. It is widely suspected, but unproven, that the tight correlation in mass of the black hole and stellar components results from the AGN quenching the surrounding star formation as it approaches its peak luminosity. X-rays trace emission from AGN unambiguously, while powerful star-forming galaxies are usually dust-obscured and are brightest at infrared to submillimetre wavelengths. Here we report observations in the submillimetre and X-ray which show that rapid star formation was common in the host galaxies of AGN when the Universe was 2-6 Gyrs old, but that the most vigorous star formation is not observed around black holes above an X-ray luminosity of 10^44 erg/s. This suppression of star formation in the host galaxies of powerful AGN is a key prediction of models in which the AGN drives a powerful outflow, expelling the interstellar medium of its host galaxy and transforming the galaxy's properties in a brief period of cosmic time., Comment: Published in Nature, May 2012. Includes supplementary information

Published
2013
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50. Flux calibration of the Herschel-SPIRE photometer

Author

Bendo, G. J., Griffin, M. J., Bock, J. J., Conversi, L., Dowell, C. D., Lim, T., Lu, N., North, C. E., Papageorgiou, A., Pearson, C. P., Pohlen, M., Polehampton, E. T., Schulz, B., Shupe, D. L., Sibthorpe, B., Spencer, L. D., Swinyard, B. M., Valtchanov, I., Xu, C. K., Bendo, G. J., Griffin, M. J., Bock, J. J., Conversi, L., Dowell, C. D., Lim, T., Lu, N., North, C. E., Papageorgiou, A., Pearson, C. P., Pohlen, M., Polehampton, E. T., Schulz, B., Shupe, D. L., Sibthorpe, B., Spencer, L. D., Swinyard, B. M., Valtchanov, I., and Xu, C. K.

Abstract

We describe the procedure used to flux calibrate the three-band submillimetre photometer in the Spectral and Photometric Imaging REceiver (SPIRE) instrument on the Herschel Space Observatory. This includes the equations describing the calibration scheme, a justification for using Neptune as the primary calibration source, a description of the observations and data processing procedures used to derive flux calibration parameters (for converting from voltage to flux density) for every bolometer in each array, an analysis of the error budget in the flux calibration for the individual bolometers, and tests of the flux calibration on observations of primary and secondary calibrators. The procedure for deriving the flux calibration parameters is divided into two parts. In the first part, we use observations of astronomical sources in conjunction with the operation of the photometer internal calibration source to derive the unscaled derivatives of the flux calibration curves. To scale the calibration curves in Jy/beam/V, we then use observations of Neptune in which the beam of each bolometer is mapped using Neptune observed in a very fine scan pattern. The total instrumental uncertainties in the flux calibration for the individual bolometers is ~0.5% for most bolometers, although a few bolometers have uncertainties of ~1-5% because of issues with the Neptune observations. Based on application of the flux calibration parameters to Neptune observations performed using typical scan map observing modes, we determined that measurements from each array as a whole have instrumental uncertainties of 1.5%. This is considerably less than the absolute calibration uncertainty associated with the model of Neptune, which is estimated at 4%., Comment: 20 pages, 17 figures, accepted for publication in MNRAS

Published
2013
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