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894 results on '"De Boer, T."'

51. Four and one more: The formation history and total mass of globular clusters in the Fornax dSph

Author

de Boer, T. J. L. and Fraser, M.

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

We have determined the detailed star formation history and total mass of the globular clusters in the Fornax dwarf spheroidal using archival HST WFPC2 data. Colour magnitude diagrams are constructed in the F555W and F814W bands and corrected for the effect of Fornax field star contamination, after which we use the routine Talos to derive the quantitative star formation history as a function of age and metallicity. The star formation history of the Fornax globular clusters shows that Fornax 1, 2, 3 and 5 are all dominated by ancient (>10 Gyr) populations. Cluster Fornax 1,2 and 3 display metallicities as low as [Fe/H]=-2.5 while Fornax 5 is slightly more metal-rich at [Fe/H]=-1.8, consistent with resolved and unresolved metallicity tracers. Conversely, Fornax 4 is dominated by a more metal-rich~([Fe/H]=-1.2) and younger population at 10 Gyr, inconsistent with the other clusters. A lack of stellar populations overlapping with the main body of Fornax argues against the nucleus cluster scenario for Fornax 4. The combined stellar mass in globular clusters as derived from the SFH is (9.57$\pm$0.93)$\times$10$^{5}$ M$_{\odot}$ which corresponds to 2.5$\pm$0.2 percent of the total stellar mass in Fornax. The mass of the four most metal-poor clusters can be further compared to the metal-poor Fornax field to yield a mass fraction of 19.6$\pm$3.1 percent. Therefore, the SFH results provide separate supporting evidence for the unusually high mass fraction of the GCs compared to the Fornax field population., Comment: 11 pages, 11 figures. Accepted in A&A

Published
2015
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52. The star formation history of the Sagittarius stream

Author

de Boer, T. J. L., Belokurov, V., and Koposov, S.

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

We present the first detailed quantitative study of the stellar populations of the Sagittarius (Sgr) streams within the Stripe 82 region, using photometric and spectroscopic observations from the Sloan Digital Sky Survey (SDSS). The star formation history (SFH) is determined separately for the bright and faint Sgr streams, to establish whether both components consist of a similar stellar population mix or have a distinct origin. Best fit SFH solutions are characterised by a well-defined, tight sequence in age-metallicity space, indicating that star formation occurred within a well-mixed, homogeneously enriched medium. Star formation rates dropped sharply at an age of ~5-7 Gyr, possibly related to the accretion of Sgr by the MW. Finally, the Sgr sequence displays a change of slope in age-metallicity space at an age between 11-13 Gyr consistent with the Sgr alpha-element knee, indicating that supernovae type Ia started contributing to the abundance pattern ~1-3 Gyr after the start of star formation. Results for both streams are consistent with being drawn from the parent Sgr population mix, but at different epochs. The SFH of the bright stream starts from old, metal-poor populations and extends to a metallicity of [Fe/H]~-0.7, with peaks at ~7 and 11 Gyr. The faint SFH samples the older, more metal-poor part of the Sgr sequence, with a peak at ancient ages and stars mostly with [Fe/H]<-1.3 and age>9 Gyr. Therefore, we argue in favour of a scenario where the faint stream consists of material stripped i) earlier, and ii) from the outskirts of the Sgr dwarf., Comment: 15 pages, 12 figures. ccepted for publication in MNRAS

Published
2015

53. GW190425: Pan-STARRS and ATLAS coverage of the skymap and limits on optical emission associated with FRB 20190425A

Author

Smartt, S J, primary, Nicholl, M, additional, Srivastav, S, additional, Huber, M E, additional, Chambers, K C, additional, Smith, K W, additional, Young, D R, additional, Fulton, M D, additional, Tonry, J L, additional, Stubbs, C W, additional, Denneau, L, additional, Cooper, A J, additional, Aamer, A, additional, Anderson, J P, additional, Andersson, A, additional, Bulger, J, additional, Chen, T -W, additional, Clark, P, additional, de Boer, T, additional, Gao, H, additional, Gillanders, J H, additional, Lawrence, A, additional, Lin, C C, additional, Lowe, T B, additional, Magnier, E A, additional, Minguez, P, additional, Moore, T, additional, Rest, A, additional, Shingles, L, additional, Siverd, R, additional, Smith, I A, additional, Stalder, B, additional, Stevance, H F, additional, Wainscoat, R, additional, and Williams, R, additional

Published
2024
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54. VLT/FLAMES spectroscopy of red giant branch stars in the Fornax dwarf spheroidal galaxy

Author

Lemasle, B., de Boer, T., Hill, V., Tolstoy, E., Irwin, M., Jablonka, P., Venn, K., Battaglia, G., Starkenburg, E., Shetrone, M., Letarte, B., Francois, P., Helmi, A., Primas, F., Kaufer, A., and Szeifert, T.

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

Fornax is one of the most massive dwarf spheroidal galaxies in the Local Group. The Fornax field star population is dominated by intermediate age stars but star formation was going on over almost its entire history. It has been proposed that Fornax experienced a minor merger event. Despite recent progress, only the high metallicity end of Fornax field stars ([Fe/H]>-1.2 dex) has been sampled in larger number via high resolution spectroscopy. We want to better understand the full chemical evolution of this galaxy by better sampling the whole metallicity range, including more metal poor stars. We use the VLT-FLAMES multi-fibre spectrograph in high-resolution mode to determine the abundances of several alpha, iron-peak and neutron-capture elements in a sample of 47 individual Red Giant Branch stars in the Fornax dwarf spheroidal galaxy. We combine these abundances with accurate age estimates derived from the age probability distribution from the colour-magnitude diagram of Fornax. Similar to other dwarf spheroidal galaxies, the old, metal-poor stars of Fornax are typically alpha-rich while the young metal-rich stars are alpha-poor. In the classical scenario of the time delay between SNe II and SNe Ia, we confirm that SNe Ia started to contribute to the chemical enrichment at [Fe/H] between -2.0 and -1.8 dex. We find that the onset of SNe Ia took place between 12-10 Gyrs ago. The high values of [Ba/Fe], [La/Fe] reflect the influence of SNe Ia and AGB stars in the abundance pattern of the younger stellar population of Fornax. Our findings of low [alpha/Fe] and enhanced [Eu/Mg] are compatible with an initial mass function that lacks the most massive stars and with star formation that kept going on throughout the whole history of Fornax. We find that massive stars kept enriching the interstellar medium in alpha-elements, although they were not the main contributor to the iron enrichment., Comment: Resubmitted to A&A (18/09/2014) after Referee's comments

Published
2014
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55. The episodic Star Formation History of the Carina Dwarf Spheroidal Galaxy

Author

de Boer, T. J. L., Tolstoy, E., Lemasle, B., Saha, A., Olszewski, E. W., Mateo, M., Irwin, M. J., and Battaglia, G.

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

We present deep photometry of the Carina dwarf Spheroidal galaxy in the B,V filters from CTIO/MOSAIC, out to and beyond the tidal radius. The accurately calibrated photometry is combined with spectroscopic metallicity distributions of Red Giant Branch stars to determine the detailed star formation and chemical evolution history. The star formation history confirms the episodic formation history of Carina and quantifies the duration and strength of each episode in great detail, as a function radius from the centre. Two main episodes of star formation occurred at old (>8 Gyr) and intermediate (2-8 Gyr) ages, both enriching stars starting from low metallicities ([Fe/H]<-2 dex). By dividing the SFH into two components, we determine that 60pm9 percent of the total number of stars formed within the intermediate age episode. Furthermore, within the tidal radius (0.48 degrees or 888 pc) a total mass in stars of 1.07pm0.08 x10^6 M_sun was formed, giving Carina a stellar mass-to-light ratio of 1.8pm0.8. Combining the detailed star formation history with spectroscopic observations of RGB stars, we are able to determine the detailed age-metallicity relation of each episode and the timescale of alpha-element evolution of Carina from individual stars. The oldest episode displays a tight age-metallicity relation over 6 Gyr with steadily declining alpha-element abundances and a possible alpha-element knee at [Fe/H]~ -2.5 dex. The intermediate age sequence displays a more complex age-metallicity relation starting from low metallicity and a sequence in alpha-element abundances with a slope much steeper than observed in the old episode, starting from [Fe/H]=-1.8 dex and [Mg/Fe]~0.4 dex and declining to Mg-poor values ([Mg/Fe]<-0.5 dex). This indicates clearly that both episodes of star formation formed from gas with different abundance patterns, inconsistent with simple evolution in an isolated system., Comment: accepted for publication in A&A. 14 pages, 17 figures

Published
2014
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56. The Alpha-element knee of the Sagittarius Stream

Author

de Boer, T. J. L., Belokurov, V., Beers, T. C., and Lee, Y. S.

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

We employ abundances from the Sloan Digital Sky Survey (SDSS) and the Sloan Extension for Galactic Understanding and Exploration (SEGUE) to study the alpha-element distribution of the stellar members of the Sagittarius stream. To test the reliability of SDSS/SEGUE abundances for the study of Sagittarius, we select high-likelihood samples tracing the different components of the Milky Way, and recover known literature alpha-element distributions. Using selection criteria based on the spatial position, radial velocity, distance and colours of individual stars, we obtain a robust sample of Sagittarius-stream stars. The alpha-element distribution of the Sagittarius stream forms a narrow sequence at intermediate metallicities with a clear turn-down, consistent with the presence of an alpha-element "knee". This is the first time that the alpha-element knee of the Sagittarius dwarf galaxy has been detected. Fitting a toy model to our data, we determine that the alpha-knee in Sagittarius takes place at [Fe/H]=-1.27pm0.05, only slightly less metal-poor than the knee in the Milky Way. This indicates that a small number of Sagittarius-like galaxies could have contributed significantly to the build-up of the Milky Way's stellar halo system at ancient times., Comment: 6 pages, 3 figures

Published
2014
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58. A new study of stellar substructures in the Fornax dwarf spheroidal galaxy

Author

de Boer, T. J. L., Tolstoy, E., Saha, A., and Olszewski, E. W.

Subjects
Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Using deep V, B-V wide-field photometry, we have conducted a new study of stellar over-densities in the Fornax dwarf spheroidal galaxy by determining detailed Star Formation Histories from Colour-Magnitude Diagram analysis. We have concentrated on the relatively young stellar component (<4 Gyr old), and compared this to the underlying Fornax field population. We have studied in more detail the previously known inner shell-like structure and shown that it has a well-defined age-metallicity relation with a peak at ~1.5 Gyr, [Fe/H]=-0.6 dex. Comparison to the Fornax centre shows that the over-dense feature is consistent with the age-metallicity relation of young field stars, and likely formed from Fornax gas. This is consistent with a scenario in which the over-density was formed by the re-accretion of previously expelled gas. We have also discovered a new stellar over-density, located 0.3 degrees (0.7 kpc) from the centre, which is only 100 Myr old, with solar metallicity. This feature constitutes some of the youngest, most metal-rich stars stars observed in Fornax to date. It is unclear how the young over-density was formed, although the age and metallicity of stars suggest this feature may represent the last star formation activity of the Fornax dSph., Comment: Accepted for publication in Astronomy & Astrophysics

Published
2013
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59. The Star Formation & Chemical Evolution History of the Fornax Dwarf Spheroidal Galaxy

Author

de Boer, T. J. L., Tolstoy, E., Hill, V., Saha, A., Olszewski, E. W., Mateo, M., Starkenburg, E., Battaglia, G., and Walker, M. G.

Subjects
Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We present deep photometry in the B,V and I filters from CTIO/MOSAIC for about 270.000 stars in the Fornax dwarf Spheroidal galaxy, out to a radius of r_ell\sim0.8 degrees. By combining the accurately calibrated photometry with the spectroscopic metallicity distributions of individual Red Giant Branch stars we obtain the detailed star formation and chemical evolution history of Fornax. Fornax is dominated by intermediate age (1-10 Gyr) stellar populations, but also includes ancient (10-14 Gyr), and young (<1 Gyr) stars. We show that Fornax displays a radial age gradient, with younger, more metal-rich populations dominating the central region. This confirms results from previous works. Within an elliptical radius of 0.8 degrees, or 1.9 kpc from the centre, a total mass in stars of 4.3x10^7 Msun was formed, from the earliest times until 250 Myr ago. Using the detailed star formation history, age estimates are determined for individual stars on the upper RGB, for which spectroscopic abundances are available, giving an age-metallicity relation of the Fornax dSph from individual stars. This shows that the average metallicity of Fornax went up rapidly from [Fe/H]<-2.5 dex to [Fe/H]=-1.5 dex between 8-12 Gyr ago, after which a more gradual enrichment resulted in a narrow, well-defined sequence which reaches [Fe/H]\sim-0.8 dex, \sim3 Gyr ago. These ages also allow us to measure the build-up of chemical elements as a function of time, and thus determine detailed timescales for the evolution of individual chemical elements. A rapid decrease in [Mg/Fe] is seen for the stars with [Fe/H]>-1.5 dex, with a clear trend in age., Comment: 18 pages, 20 figures

Published
2012
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60. The Star Formation & Chemical Evolution History of the Sculptor Dwarf Spheroidal Galaxy

Author

de Boer, T. J. L., Tolstoy, E., Hill, V., Saha, A., Olsen, K., Starkenburg, E., Lemasle, B., Irwin, M. J., and Battaglia, G.

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We have combined deep photometry in the B,V and I bands from CTIO/MOSAIC of the Sculptor dwarf spheroidal galaxy, going down to the oldest Main Sequence Turn-Offs, with spectroscopic metallicity distributions of Red Giant Branch stars. This allows us to obtain the most detailed and complete Star Formation History to date, as well as an accurate timescale for chemical enrichment. The Star Formation History shows that Sculptor is dominated by old ($>$10 Gyr), metal-poor stars, but that younger, more metal-rich populations are also present. Using Star Formation Histories determined at different radii from the centre we show that Sculptor formed stars with an increasing central concentration with time. The old, metal-poor populations are present at all radii, while more metal-rich, younger stars are more centrally concentrated. We find that within an elliptical radius of 1 degree, or 1.5 kpc from the centre, a total mass in stars of 7.8$\times10^{6}$ M$_{\odot}$ was formed, between 14 and 7 Gyr ago, with a peak at 13$-$14 Gyr ago. We use the detailed Star Formation History to determine age estimates for individual Red Giant Branch stars with high resolution spectroscopic abundances. Thus, for the first time, we can directly determine detailed timescales for the evolution of individual chemical elements. We find that the trends in alpha-elements match what is expected from an extended, relatively uninterrupted period of star formation continuing for 6$-$7 Gyr. The knee in the alpha-element distribution occurs at an age of 10.9$\pm$1Gyr, suggesting that SNe Ia enrichment began $\approx2\pm$1Gyr after the start of star formation in Sculptor., Comment: 23 pages, 23 figures

Published
2012
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61. VLT/FLAMES spectroscopy of Red Giant Branch stars in the Carina dwarf spheroidal galaxy

Author

Lemasle, B., Hill, V., Tolstoy, E., Venn, K. A., Shetrone, M. D., Irwin, M. J., de Boer, T. J. L., Starkenburg, E., and Salvadori, S.

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

The ages of individual Red Giant Branch stars (RGB) can range from 1 Gyr old to the age of the Universe, and it is believed that the abundances of most chemical elements in their photospheres remain unchanged with time (those that are not affected by the 1st dredge-up). This means that they trace the ISM in the galaxy at the time the star formed, and hence the chemical enrichment history of the galaxy. CMD analysis has shown the Carina dwarf spheroidal (dSph) to have had an unusually episodic star formation history (SFH) which is expected to be reflected in the abundances of different chemical elements. We use the VLT-FLAMES spectrograph in HR mode (R~20000) to measure the abundances of several chemical elements in a sample of 35 RGB stars in Carina. We also combine these abundances with photometry to derive age estimates for these stars. This allows us to determine which of two distinct star formation (SF) episodes the stars in our sample belong to, and thus to define the relationship between SF and chemical enrichment during these two episodes. As is expected from the SFH, Carina contains two distinct populations of RGB stars: one old (>10 Gyr), which we have found to be metal-poor ([Fe/H]<-1.5), and alpha-rich ([Mg/Fe]>0.0); the other intermediate age (~2-6 Gyr), which we have found to have a metallicity range (-1.8<[Fe/H]<-1.2) with a large spread in [alpha/Fe] abundance, going from extremely low values ([Mg/Fe]<-0.3) to the same mean values as the older population (<[Mg/Fe]>~0.3). We show that the chemical enrichment history of the Carina dSph was different for each SF episode. The earliest was short (~2-3 Gyr) and resulted in the rapid chemical enrichment of the whole galaxy to [Fe/H] ~ -1.5 with both SNe II and SNe Ia contributions. The subsequent episode occured after a gap of ~3-4 Gyr and appears to have resulted in relatively little evolution in either [Fe/H] or [alpha/Fe]., Comment: Accepted in A&A

Published
2011
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62. Deep Wide-Field Imaging down to the oldest Main Sequence Turnoffs in the Sculptor dwarf spheroidal galaxy

Author

de Boer, T. J. L., Tolstoy, E., Saha, A., Olsen, K., Irwin, M. J., Battaglia, G., Hill, V., Shetrone, M. D., Fiorentino, G., and Cole, A.

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We present wide-field photometry of resolved stars in the nearby Sculptor dwarf spheroidal galaxy using CTIO/MOSAIC, going down to the oldest Main Sequence Turn-Off. The accurately flux calibrated wide field Colour-Magnitude Diagrams can be used to constrain the ages of different stellar populations, and also their spatial distribution. The Sculptor dSph contains a predominantly ancient stellar population (>10 Gyr old) which can be easily resolved into individual stars. A galaxy dominated by an old population provides a clear view of ancient processes of galaxy formation unimpeded by overlying younger populations. By using spectroscopic metallicities of RGB stars in combination with our deep Main Sequence Turn-Off photometry we can constrain the ages of different stellar populations with particular accuracy. We find that the known metallicity gradient in Sculptor is well matched to an age gradient. This is the first time that this link with age has been directly quantified. This gradient has been previously observed as a variation in Horizontal Branch properties and is now confirmed to exist for Main Sequence Turn-Offs as well. It is likely the Sculptor dSph first formed an extended metal-poor population at the oldest times, and subsequent more metal-rich, younger stars were formed more towards the centre until the gas was depleted or lost roughly 7 Gyr ago. The fact that these clear radial gradients have been preserved up to the present day is consistent with the apparent lack of signs of recent tidal interactions., Comment: 28 pages, 22 figures

Published
2011
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63. AT 2022aedm and a New Class of Luminous, Fast-cooling Transients in Elliptical Galaxies

Author

Nicholl, M., primary, Srivastav, S., additional, Fulton, M. D., additional, Gomez, S., additional, Huber, M. E., additional, Oates, S. R., additional, Ramsden, P., additional, Rhodes, L., additional, Smartt, S. J., additional, Smith, K. W., additional, Aamer, A., additional, Anderson, J. P., additional, Bauer, F. E., additional, Berger, E., additional, de Boer, T., additional, Chambers, K. C., additional, Charalampopoulos, P., additional, Chen, T.-W., additional, Fender, R. P., additional, Fraser, M., additional, Gao, H., additional, Green, D. A., additional, Galbany, L., additional, Gompertz, B. P., additional, Gromadzki, M., additional, Gutiérrez, C. P., additional, Howell, D. A., additional, Inserra, C., additional, Jonker, P. G., additional, Kopsacheili, M., additional, Lowe, T. B., additional, Magnier, E. A., additional, McCully, C., additional, McGee, S. L., additional, Moore, T., additional, Müller-Bravo, T. E., additional, Newsome, M., additional, Gonzalez, E. Padilla, additional, Pellegrino, C., additional, Pessi, T., additional, Pursiainen, M., additional, Rest, A., additional, Ridley, E. J., additional, Shappee, B. J., additional, Sheng, X., additional, Smith, G. P., additional, Terreran, G., additional, Tucker, M. A., additional, Vinkó, J., additional, Wainscoat, R. J., additional, Wiseman, P., additional, and Young, D. R., additional

Published
2023
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64. Panning for gold, but finding helium: Discovery of the ultra-stripped supernova SN 2019wxt from gravitational-wave follow-up observations

Author

Agudo, I., primary, Amati, L., additional, An, T., additional, Bauer, F. E., additional, Benetti, S., additional, Bernardini, M. G., additional, Beswick, R., additional, Bhirombhakdi, K., additional, de Boer, T., additional, Branchesi, M., additional, Brennan, S. J., additional, Brocato, E., additional, Caballero-García, M. D., additional, Cappellaro, E., additional, Castro Rodríguez, N., additional, Castro-Tirado, A. J., additional, Chambers, K. C., additional, Chassande-Mottin, E., additional, Chaty, S., additional, Chen, T.-W., additional, Coleiro, A., additional, Covino, S., additional, D’Ammando, F., additional, D’Avanzo, P., additional, D’Elia, V., additional, Fiore, A., additional, Flörs, A., additional, Fraser, M., additional, Frey, S., additional, Frohmaier, C., additional, Fulton, M., additional, Galbany, L., additional, Gall, C., additional, Gao, H., additional, García-Rojas, J., additional, Ghirlanda, G., additional, Giarratana, S., additional, Gillanders, J. H., additional, Giroletti, M., additional, Gompertz, B. P., additional, Gromadzki, M., additional, Heintz, K. E., additional, Hjorth, J., additional, Hu, Y.-D., additional, Huber, M. E., additional, Inkenhaag, A., additional, Izzo, L., additional, Jin, Z. P., additional, Jonker, P. G., additional, Kann, D. A., additional, Kool, E. C., additional, Kotak, R., additional, Leloudas, G., additional, Levan, A. J., additional, Lin, C.-C., additional, Lyman, J. D., additional, Magnier, E. A., additional, Maguire, K., additional, Mandel, I., additional, Marcote, B., additional, Mata Sánchez, D., additional, Mattila, S., additional, Melandri, A., additional, Michałowski, M. J., additional, Moldon, J., additional, Nicholl, M., additional, Nicuesa Guelbenzu, A., additional, Oates, S. R., additional, Onori, F., additional, Orienti, M., additional, Paladino, R., additional, Paragi, Z., additional, Perez-Torres, M., additional, Pian, E., additional, Pignata, G., additional, Piranomonte, S., additional, Quirola-Vásquez, J., additional, Ragosta, F., additional, Rau, A., additional, Ronchini, S., additional, Rossi, A., additional, Sánchez-Ramírez, R., additional, Salafia, O. S., additional, Schulze, S., additional, Smartt, S. J., additional, Smith, K. W., additional, Sollerman, J., additional, Srivastav, S., additional, Starling, R. L. C., additional, Steeghs, D., additional, Stevance, H. F., additional, Tanvir, N. R., additional, Testa, V., additional, Torres, M. A. P., additional, Valeev, A., additional, Vergani, S. D., additional, Vescovi, D., additional, Wainscost, R., additional, Watson, D., additional, Wiersema, K., additional, Wyrzykowski, Ł., additional, Yang, J., additional, Yang, S., additional, and Young, D. R., additional

Published
2023
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66. SN 2022ann: a Type Icn supernova from a dwarf galaxy that reveals helium in its circumstellar environment

Author

Davis, K W, primary, Taggart, K, additional, Tinyanont, S, additional, Foley, R J, additional, Villar, V A, additional, Izzo, L, additional, Angus, C R, additional, Bustamante-Rosell, M J, additional, Coulter, D A, additional, Earl, N, additional, Farias, D, additional, Hjorth, J, additional, Huber, M E, additional, Jones, D O, additional, Kelly, P L, additional, Kilpatrick, C D, additional, Langeroodi, D, additional, Miao, H-Y, additional, Pellegrino, C M, additional, Ramirez-Ruiz, E, additional, Ransome, C L, additional, Rest, S, additional, Siebert, M R, additional, Terreran, G, additional, Thornton, I M, additional, Yadavalli, S K, additional, Zeimann, G R, additional, Auchettl, K, additional, Bom, C R, additional, Brink, T G, additional, Burke, J, additional, Camacho-Neves, Y, additional, Chambers, K C, additional, de Boer, T J L, additional, DeMarchi, L, additional, Filippenko, A V, additional, Galbany, L, additional, Gall, C, additional, Gao, H, additional, Herpich, F R, additional, Howell, D A, additional, Jacobson-Galan, W V, additional, Jha, S W, additional, Kanaan, A, additional, Khetan, N, additional, Kwok, L A, additional, Lai, Z, additional, Larison, C, additional, Lin, C-C, additional, Loertscher, K C, additional, Magnier, E A, additional, McCully, C, additional, McGill, P, additional, Newsome, M, additional, Padilla Gonzalez, E, additional, Pan, Y-C, additional, Rest, A, additional, Rho, J, additional, Ribeiro, T, additional, Santos, A, additional, Schoenell, W, additional, Sharief, S N, additional, Smith, K W, additional, Wainscoat, R J, additional, Wang, Q, additional, Zenati, Y, additional, and Zheng, W, additional

Published
2023
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67. The Young Supernova Experiment Data Release 1 (YSE DR1): Light Curves and Photometric Classification of 1975 Supernovae

Author

Aleo, P. D., primary, Malanchev, K., additional, Sharief, S., additional, Jones, D. O., additional, Narayan, G., additional, Foley, R. J., additional, Villar, V. A., additional, Angus, C. R., additional, Baldassare, V. F., additional, Bustamante-Rosell, M. J., additional, Chatterjee, D., additional, Cold, C., additional, Coulter, D. A., additional, Davis, K. W., additional, Dhawan, S., additional, Drout, M. R., additional, Engel, A., additional, French, K. D., additional, Gagliano, A., additional, Gall, C., additional, Hjorth, J., additional, Huber, M. E., additional, Jacobson-Galán, W. V., additional, Kilpatrick, C. D., additional, Langeroodi, D., additional, Macias, P., additional, Mandel, K. S., additional, Margutti, R., additional, Matasić, F., additional, McGill, P., additional, Pierel, J. D. R., additional, Ramirez-Ruiz, E., additional, Ransome, C. L., additional, Rojas-Bravo, C., additional, Siebert, M. R., additional, Smith, K. W., additional, de Soto, K. M., additional, Stroh, M. C., additional, Tinyanont, S., additional, Taggart, K., additional, Ward, S. M., additional, Wojtak, R., additional, Auchettl, K., additional, Blanchard, P. K., additional, de Boer, T. J. L., additional, Boyd, B. M., additional, Carroll, C. M., additional, Chambers, K. C., additional, DeMarchi, L., additional, Dimitriadis, G., additional, Dodd, S. A., additional, Earl, N., additional, Farias, D., additional, Gao, H., additional, Gomez, S., additional, Grayling, M., additional, Grillo, C., additional, Hayes, E. E., additional, Hung, T., additional, Izzo, L., additional, Khetan, N., additional, Kolborg, A. N., additional, Law-Smith, J. A. P., additional, LeBaron, N., additional, Lin, C.-C., additional, Luo, Y., additional, Magnier, E. A., additional, Matthews, D., additional, Mockler, B., additional, O’Grady, A. J. G., additional, Pan, Y.-C., additional, Politsch, C. A., additional, Raimundo, S. I., additional, Rest, A., additional, Ridden-Harper, R., additional, Sarangi, A., additional, Schrøder, S. L., additional, Smartt, S. J., additional, Terreran, G., additional, Thorp, S., additional, Vazquez, J., additional, Wainscoat, R. J., additional, Wang, Q., additional, Wasserman, A. R., additional, Yadavalli, S. K., additional, Yarza, R., additional, and Zenati, Y., additional

Published
2023
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68. A UNIONS view of the brightest central galaxies of candidate fossil groups

Author

Chu, A., primary, Durret, F., additional, Ellien, A., additional, Sarron, F., additional, Adami, C., additional, Márquez, I., additional, Martinet, N., additional, de Boer, T., additional, Chambers, K. C., additional, Cuillandre, J.-C., additional, Gwyn, S., additional, Magnier, E. A., additional, and McConnachie, A. W., additional

Published
2023
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69. The Optical Light Curve of GRB 221009A: The Afterglow and the Emerging Supernova

Author

Fulton, M. D., primary, Smartt, S. J., additional, Rhodes, L., additional, Huber, M. E., additional, Villar, V. A., additional, Moore, T., additional, Srivastav, S., additional, Schultz, A. S. B., additional, Chambers, K. C., additional, Izzo, L., additional, Hjorth, J., additional, Chen, T.-W., additional, Nicholl, M., additional, Foley, R. J., additional, Rest, A., additional, Smith, K. W., additional, Young, D. R., additional, Sim, S. A., additional, Bright, J., additional, Zenati, Y., additional, de Boer, T., additional, Bulger, J., additional, Fairlamb, J., additional, Gao, H., additional, Lin, C.-C., additional, Lowe, T., additional, Magnier, E. A., additional, Smith, I. A., additional, Wainscoat, R., additional, Coulter, D. A., additional, Jones, D. O., additional, Kilpatrick, C. D., additional, McGill, P., additional, Ramirez-Ruiz, E., additional, Lee, K.-S., additional, Narayan, G., additional, Ramakrishnan, V., additional, Ridden-Harper, R., additional, Singh, A., additional, Wang, Q., additional, Kong, A. K. H., additional, Ngeow, C.-C., additional, Pan, Y.-C., additional, Yang, S., additional, Davis, K. W., additional, Piro, A. L., additional, Rojas-Bravo, C., additional, Sommer, J., additional, and Yadavalli, S. K., additional

Published
2023
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70. Forbidden hugs in pandemic times

Author

Pastorello, A., primary, Valerin, G., additional, Fraser, M., additional, Reguitti, A., additional, Elias-Rosa, N., additional, Filippenko, A. V., additional, Rojas-Bravo, C., additional, Tartaglia, L., additional, Reynolds, T. M., additional, Valenti, S., additional, Andrews, J. E., additional, Ashall, C., additional, Bostroem, K. A., additional, Brink, T. G., additional, Burke, J., additional, Cai, Y.-Z., additional, Cappellaro, E., additional, Coulter, D. A., additional, Dastidar, R., additional, Davis, K. W., additional, Dimitriadis, G., additional, Fiore, A., additional, Foley, R. J., additional, Fugazza, D., additional, Galbany, L., additional, Gangopadhyay, A., additional, Geier, S., additional, Gutiérrez, C. P., additional, Haislip, J., additional, Hiramatsu, D., additional, Holmbo, S., additional, Howell, D. A., additional, Hsiao, E. Y., additional, Hung, T., additional, Jha, S. W., additional, Kankare, E., additional, Karamehmetoglu, E., additional, Kilpatrick, C. D., additional, Kotak, R., additional, Kouprianov, V., additional, Kravtsov, T., additional, Kumar, S., additional, Li, Z.-T., additional, Lundquist, M. J., additional, Lundqvist, P., additional, Matilainen, K., additional, Mazzali, P. A., additional, McCully, C., additional, Misra, K., additional, Morales-Garoffolo, A., additional, Moran, S., additional, Morrell, N., additional, Newsome, M., additional, Padilla Gonzalez, E., additional, Pan, Y.-C., additional, Pellegrino, C., additional, Phillips, M. M., additional, Pignata, G., additional, Piro, A. L., additional, Reichart, D. E., additional, Rest, A., additional, Salmaso, I., additional, Sand, D. J., additional, Siebert, M. R., additional, Smartt, S. J., additional, Smith, K. W., additional, Srivastav, S., additional, Stritzinger, M. D., additional, Taggart, K., additional, Tinyanont, S., additional, Yan, S.-Y., additional, Wang, L., additional, Wang, X.-F., additional, Williams, S. C., additional, Wyatt, S., additional, Zhang, T.-M., additional, de Boer, T., additional, Chambers, K., additional, Gao, H., additional, and Magnier, E., additional

Published
2023
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71. The Young Supernova Experiment Data Release 1 (YSE DR1):Light Curves and Photometric Classification of 1975 Supernovae

Author

Aleo, P. D., Malanchev, K., Sharief, S., Jones, D. O., Narayan, G., Foley, R. J., Villar, V. A., Angus, C. R., Baldassare, V. F., Bustamante-Rosell, M. J., Chatterjee, D., Cold, C., Coulter, D. A., Davis, K. W., Dhawan, S., Drout, M. R., Engel, A., French, K. D., Gagliano, A., Gall, C., Hjorth, J., Huber, M. E., Jacobson-Galan, W. V., Kilpatrick, C. D., Langeroodi, D., Macias, P., Mandel, K. S., Margutti, R., Matasic, F., McGill, P., Pierel, J. D. R., Ramirez-Ruiz, E., Ransome, C. L., Rojas-Bravo, C., Siebert, M. R., Smith, K. W., de Soto, K. M., Stroh, M. C., Tinyanont, S., Taggart, K., Ward, S. M., Wojtak, R., Auchettl, K., Blanchard, P. K., de Boer, T. J. L., Boyd, B. M., Carroll, C. M., Chambers, K. C., DeMarchi, L., Dimitriadis, G., Dodd, S. A., Earl, N., Farias, D., Gao, H., Gomez, S., Grayling, M., Grillo, C., Hayes, E. E., Hung, T., Izzo, L., Khetan, N., Kolborg, A. N., Law-Smith, J. A. P., LeBaron, N., Lin, C. -c., Luo, Y., Magnier, E. A., Matthews, D., Mockler, B., O'Grady, A. J. G., Pan, Y. -c., Politsch, C. A., Raimundo, S. I., Rest, A., Ridden-Harper, R., Sarangi, A., Schroder, S. L., Smartt, S. J., Terreran, G., Thorp, S., Vazquez, J., Wainscoat, R. J., Wang, Q., Wasserman, A. R., Yadavalli, S. K., Yarza, R., Zenati, Y., Aleo, P. D., Malanchev, K., Sharief, S., Jones, D. O., Narayan, G., Foley, R. J., Villar, V. A., Angus, C. R., Baldassare, V. F., Bustamante-Rosell, M. J., Chatterjee, D., Cold, C., Coulter, D. A., Davis, K. W., Dhawan, S., Drout, M. R., Engel, A., French, K. D., Gagliano, A., Gall, C., Hjorth, J., Huber, M. E., Jacobson-Galan, W. V., Kilpatrick, C. D., Langeroodi, D., Macias, P., Mandel, K. S., Margutti, R., Matasic, F., McGill, P., Pierel, J. D. R., Ramirez-Ruiz, E., Ransome, C. L., Rojas-Bravo, C., Siebert, M. R., Smith, K. W., de Soto, K. M., Stroh, M. C., Tinyanont, S., Taggart, K., Ward, S. M., Wojtak, R., Auchettl, K., Blanchard, P. K., de Boer, T. J. L., Boyd, B. M., Carroll, C. M., Chambers, K. C., DeMarchi, L., Dimitriadis, G., Dodd, S. A., Earl, N., Farias, D., Gao, H., Gomez, S., Grayling, M., Grillo, C., Hayes, E. E., Hung, T., Izzo, L., Khetan, N., Kolborg, A. N., Law-Smith, J. A. P., LeBaron, N., Lin, C. -c., Luo, Y., Magnier, E. A., Matthews, D., Mockler, B., O'Grady, A. J. G., Pan, Y. -c., Politsch, C. A., Raimundo, S. I., Rest, A., Ridden-Harper, R., Sarangi, A., Schroder, S. L., Smartt, S. J., Terreran, G., Thorp, S., Vazquez, J., Wainscoat, R. J., Wang, Q., Wasserman, A. R., Yadavalli, S. K., Yarza, R., and Zenati, Y.

Abstract

We present the Young Supernova Experiment Data Release 1 (YSE DR1), comprised of processed multicolor PanSTARRS1 griz and Zwicky Transient Facility (ZTF) gr photometry of 1975 transients with host-galaxy associations, redshifts, spectroscopic and/or photometric classifications, and additional data products from 2019 November 24 to 2021 December 20. YSE DR1 spans discoveries and observations from young and fast-rising supernovae (SNe) to transients that persist for over a year, with a redshift distribution reaching z approximate to 0.5. We present relative SN rates from YSE's magnitude- and volume-limited surveys, which are consistent with previously published values within estimated uncertainties for untargeted surveys. We combine YSE and ZTF data, and create multisurvey SN simulations to train the ParSNIP and SuperRAENN photometric classification algorithms; when validating our ParSNIP classifier on 472 spectroscopically classified YSE DR1 SNe, we achieve 82% accuracy across three SN classes (SNe Ia, II, Ib/Ic) and 90% accuracy across two SN classes (SNe Ia, core-collapse SNe). Our classifier performs particularly well on SNe Ia, with high (>90%) individual completeness and purity, which will help build an anchor photometric SNe Ia sample for cosmology. We then use our photometric classifier to characterize our photometric sample of 1483 SNe, labeling 1048 (similar to 71%) SNe Ia, 339 (similar to 23%) SNe II, and 96 (similar to 6%) SNe Ib/Ic. YSE DR1 provides a training ground for building discovery, anomaly detection, and classification algorithms, performing cosmological analyses, understanding the nature of red and rare transients, exploring tidal disruption events and nuclear variability, and preparing for the forthcoming Vera C. Rubin Observatory Legacy Survey of Space and Time.

Published
2023

72. The rise and fall of the iron-strong nuclear transient PS16dtm

Author

Petrushevska, T., Leloudas, G., Ilić, D., Bronikowski, M., Charalampopoulos, P., Jaisawal, G. K., Paraskeva, E., Pursiainen, M., Rakić, N., Schulze, Steve, Taggart, K., Wedderkopp, C. K., Anderson, J. P., de Boer, T., Chambers, K., Chen, Ting-Wan, Damljanović, G., Fraser, M., Gao, H., Gomboc, A., Gromadzki, M., Ihanec, N., Maguire, K., Marčun, B., Müller-Bravo, T. E., Nicholl, M., Onori, F., Reynolds, T. M., Smartt, S. J., Sollerman, Jesper, Smith, K. W., Wevers, T., Wyrzykowski, Ł., Petrushevska, T., Leloudas, G., Ilić, D., Bronikowski, M., Charalampopoulos, P., Jaisawal, G. K., Paraskeva, E., Pursiainen, M., Rakić, N., Schulze, Steve, Taggart, K., Wedderkopp, C. K., Anderson, J. P., de Boer, T., Chambers, K., Chen, Ting-Wan, Damljanović, G., Fraser, M., Gao, H., Gomboc, A., Gromadzki, M., Ihanec, N., Maguire, K., Marčun, B., Müller-Bravo, T. E., Nicholl, M., Onori, F., Reynolds, T. M., Smartt, S. J., Sollerman, Jesper, Smith, K. W., Wevers, T., and Wyrzykowski, Ł.

Abstract

Context. Thanks to the advent of large-scale optical surveys, a diverse set of flares from the nuclear regions of galaxies has recently been discovered. These include the disruption of stars by supermassive black holes at the centers of galaxies – nuclear transients known as tidal disruption events (TDEs). Active galactic nuclei (AGN) can show extreme changes in the brightness and emission line intensities, often referred to as changing-look AGN (CLAGN). Given the physical and observational similarities, the interpretation and distinction of nuclear transients as CLAGN or TDEs remains difficult. One of the obstacles of making progress in the field is the lack of well-sampled data of long-lived nuclear outbursts in AGN. Aims. Here, we study PS16dtm, a nuclear transient in a Narrow Line Seyfert 1 (NLSy1) galaxy, which has been proposed to be a TDE candidate. Our aim is to study the spectroscopic and photometric properties of PS16dtm, in order to better understand the outbursts originating in NLSy1 galaxies. Methods. Our extensive multiwavelength follow-up that spans around 2000 days includes photometry and spectroscopy in the UV/optical, as well as mid-infrared (MIR) and X-ray observations. Furthermore, we improved an existing semiempirical model in order to reproduce the spectra and study the evolution of the spectral lines. Results. The UV/optical light curve shows a double peak at ∼50 and ∼100 days after the first detection, and it declines and flattens afterward, reaching preoutburst levels after 2000 days of monitoring. The MIR light curve rises almost simultaneously with the optical, but unlike the UV/optical which is approaching the preoutburst levels in the last epochs of our observations, the MIR emission is still rising at the time of writing. The optical spectra show broad Balmer features and the strongest broad Fe II emission ever detected in a nuclear transient. This broad Fe II emission was not present in the archival preoutburst spectrum and almost comp

Published
2023
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73. Panning for gold, but finding helium:Discovery of the ultra-stripped supernova SN 2019wxt from gravitational-wave follow-up observations

Author

Agudo, I., Amati, L., An, T., Bauer, F.E., Benetti, S., Bernardini, M.G., Beswick, R., Bhirombhakdi, K., De Boer, T., Branchesi, M., Brennan, S.J., Brocato, E., Caballero-García, M.D., Cappellaro, E., Castro Rodríguez, N., Castro-Tirado, A.J., Chambers, K.C., Chassande-Mottin, E., Chaty, S., Chen, T.-W., Coleiro, A., Covino, S., Da'ammando, F., Da'avanzo, P., Da'elia, V., Fiore, A., Flörs, A., Fraser, M., Frey, S., Frohmaier, C., Fulton, M., Galbany, L., Gall, C., Gao, H., García-Rojas, J., Ghirlanda, G., Giarratana, S., Gillanders, J.H., Giroletti, M., Gompertz, B.P., Gromadzki, M., Heintz, K.E., Hjorth, J., Hu, Y.-D., Huber, M.E., Inkenhaag, A., Izzo, L., Jin, Z.P., Jonker, P.G., Kann, D.A., Kool, E.C., Kotak, R., Leloudas, G., Levan, A.J., Lin, C.-C., Lyman, J.D., Magnier, E.A., Maguire, K., Mandel, I., Marcote, B., Mata Sánchez, D., Mattila, S., Melandri, A., Michaåà  Owski, M.J., Moldon, J., Nicholl, M., Nicuesa Guelbenzu, A., Oates, S.R., Onori, F., Orienti, M., Paladino, R., Paragi, Z., Perez-Torres, M., Pian, E., Pignata, G., Piranomonte, S., Quirola-Vásquez, J., Ragosta, F., Rau, A., Ronchini, S., Rossi, A., Sánchez-Ramírez, R., Salafia, O.S., Schulze, S., Smartt, S.J., Smith, K.W., Sollerman, J., Srivastav, S., Starling, R.L.C., Steeghs, D., Stevance, H.F., Tanvir, N.R., Testa, V., Torres, M.A.P., Valeev, A., Vergani, S.D., Vescovi, D., Wainscost, R., Watson, D., Wiersema, K., Wyrzykowski, L., Yang, J., Yang, S., Young, D.R., Agudo, I., Amati, L., An, T., Bauer, F.E., Benetti, S., Bernardini, M.G., Beswick, R., Bhirombhakdi, K., De Boer, T., Branchesi, M., Brennan, S.J., Brocato, E., Caballero-García, M.D., Cappellaro, E., Castro Rodríguez, N., Castro-Tirado, A.J., Chambers, K.C., Chassande-Mottin, E., Chaty, S., Chen, T.-W., Coleiro, A., Covino, S., Da'ammando, F., Da'avanzo, P., Da'elia, V., Fiore, A., Flörs, A., Fraser, M., Frey, S., Frohmaier, C., Fulton, M., Galbany, L., Gall, C., Gao, H., García-Rojas, J., Ghirlanda, G., Giarratana, S., Gillanders, J.H., Giroletti, M., Gompertz, B.P., Gromadzki, M., Heintz, K.E., Hjorth, J., Hu, Y.-D., Huber, M.E., Inkenhaag, A., Izzo, L., Jin, Z.P., Jonker, P.G., Kann, D.A., Kool, E.C., Kotak, R., Leloudas, G., Levan, A.J., Lin, C.-C., Lyman, J.D., Magnier, E.A., Maguire, K., Mandel, I., Marcote, B., Mata Sánchez, D., Mattila, S., Melandri, A., Michaåà  Owski, M.J., Moldon, J., Nicholl, M., Nicuesa Guelbenzu, A., Oates, S.R., Onori, F., Orienti, M., Paladino, R., Paragi, Z., Perez-Torres, M., Pian, E., Pignata, G., Piranomonte, S., Quirola-Vásquez, J., Ragosta, F., Rau, A., Ronchini, S., Rossi, A., Sánchez-Ramírez, R., Salafia, O.S., Schulze, S., Smartt, S.J., Smith, K.W., Sollerman, J., Srivastav, S., Starling, R.L.C., Steeghs, D., Stevance, H.F., Tanvir, N.R., Testa, V., Torres, M.A.P., Valeev, A., Vergani, S.D., Vescovi, D., Wainscost, R., Watson, D., Wiersema, K., Wyrzykowski, L., Yang, J., Yang, S., and Young, D.R.

Abstract

We present the results from multi-wavelength observations of a transient discovered during an intensive follow-up campaign of S191213g, a gravitational wave (GW) event reported by the LIGO-Virgo Collaboration as a possible binary neutron star merger in a low latency search. This search yielded SN 2019wxt, a young transient in a galaxy whose sky position (in the 80% GW contour) and distance (∼150 Mpc) were plausibly compatible with the localisation uncertainty of the GW event. Initially, the transienta's tightly constrained age, its relatively faint peak magnitude (Mi ∼ -16.7 mag), and the r-band decline rate of ∼1 mag per 5 days appeared suggestive of a compact binary merger. However, SN 2019wxt spectroscopically resembled a type Ib supernova, and analysis of the optical-near-infrared evolution rapidly led to the conclusion that while it could not be associated with S191213g, it nevertheless represented an extreme outcome of stellar evolution. By modelling the light curve, we estimated an ejecta mass of only ∼0.1 M·, with 56Ni comprising ∼20% of this. We were broadly able to reproduce its spectral evolution with a composition dominated by helium and oxygen, with trace amounts of calcium. We considered various progenitor channels that could give rise to the observed properties of SN 2019wxt and concluded that an ultra-stripped origin in a binary system is the most likely explanation. Disentangling genuine electromagnetic counterparts to GW events from transients such as SN 2019wxt soon after discovery is challenging: in a bid to characterise this level of contamination, we estimated the rate of events with a volumetric rate density comparable to that of SN 2019wxt and found that around one such event per week can occur within the typical GW localisation area of O4 alerts out to a luminosity distance of 500 Mpc, beyond which it would become fainter than the typical depth of current electromagnetic follow-up campaigns.

Published
2023

74. SN 2022ann:a Type Icn supernova from a dwarf galaxy that reveals helium in its circumstellar environment

Author

Davis, K. W., Taggart, K., Tinyanont, S., Foley, R. J., Villar, V. A., Izzo, L., Angus, C. R., Bustamante-Rosell, M. J., Coulter, D. A., Earl, N., Farias, D., Hjorth, J., Huber, M. E., Jones, D. O., Kelly, P. L., Kilpatrick, C. D., Langeroodi, D., Miao, H. Y., Pellegrino, C. M., Ramirez-Ruiz, E., Ransome, C. L., Rest, S., Siebert, M. R., Terreran, G., Thornton, I. M., Yadavalli, S. K., Zeimann, G. R., Auchettl, K., Bom, C. R., Brink, T. G., Burke, J., Camacho-Neves, Y., Chambers, K. C., De Boer, T. J.L., Demarchi, L., Filippenko, A. V., Galbany, L., Gall, C., Gao, H., Herpich, F. R., Howell, D. A., Jacobson-Galan, W. V., Jha, S. W., Kanaan, A., Khetan, N., Kwok, L. A., Lai, Z., Larison, C., Lin, C. C., Loertscher, K. C., Magnier, E. A., Mccully, C., McGill, P., Newsome, M., Padilla Gonzalez, E., Pan, Y. C., Rest, A., Rho, J., Ribeiro, T., Santos, A., Schoenell, W., Sharief, S. N., Smith, K. W., Wainscoat, R. J., Wang, Q., Zenati, Y., Zheng, W., Davis, K. W., Taggart, K., Tinyanont, S., Foley, R. J., Villar, V. A., Izzo, L., Angus, C. R., Bustamante-Rosell, M. J., Coulter, D. A., Earl, N., Farias, D., Hjorth, J., Huber, M. E., Jones, D. O., Kelly, P. L., Kilpatrick, C. D., Langeroodi, D., Miao, H. Y., Pellegrino, C. M., Ramirez-Ruiz, E., Ransome, C. L., Rest, S., Siebert, M. R., Terreran, G., Thornton, I. M., Yadavalli, S. K., Zeimann, G. R., Auchettl, K., Bom, C. R., Brink, T. G., Burke, J., Camacho-Neves, Y., Chambers, K. C., De Boer, T. J.L., Demarchi, L., Filippenko, A. V., Galbany, L., Gall, C., Gao, H., Herpich, F. R., Howell, D. A., Jacobson-Galan, W. V., Jha, S. W., Kanaan, A., Khetan, N., Kwok, L. A., Lai, Z., Larison, C., Lin, C. C., Loertscher, K. C., Magnier, E. A., Mccully, C., McGill, P., Newsome, M., Padilla Gonzalez, E., Pan, Y. C., Rest, A., Rho, J., Ribeiro, T., Santos, A., Schoenell, W., Sharief, S. N., Smith, K. W., Wainscoat, R. J., Wang, Q., Zenati, Y., and Zheng, W.

Abstract

We present optical and near-infrared (NIR) observations of the Type Icn supernova (SN Icn) 2022ann, the fifth member of its newly identified class of SNe. Its early optical spectra are dominated by narrow carbon and oxygen P-Cygni features with absorption velocities of ∼800 km s-1; slower than other SNe Icn and indicative of interaction with a dense, H/He-poor circumstellar medium (CSM) that is outflowing slower than typical Wolf-Rayet wind velocities of >1000 km s-1. We identify helium in NIR spectra 2 weeks after maximum and in optical spectra at 3 weeks, demonstrating that the CSM is not fully devoid of helium. Unlike other SNe Icn, the spectra of SN 2022ann never develop broad features from SN ejecta, including in the nebular phase. Compared to other SNe Icn, SN 2022ann has a low luminosity (o-band absolute magnitude of ∼-17.7), and evolves slowly. The bolometric light curve is well-modelled by 4.8 M⊙ of SN ejecta interacting with 1.3 M⊙ of CSM. We place an upper limit of 0.04 M⊙ of 56Ni synthesized in the explosion. The host galaxy is a dwarf galaxy with a stellar mass of 107.34 M⊙ (implied metallicity of log(Z/Z⊙) ≈ 0.10) and integrated star-formation rate of log (SFR) = -2.20 M⊙ yr-1; both lower than 97 per cent of galaxies observed to produce core-collapse supernovae, although consistent with star-forming galaxies on the galaxy Main Sequence. The low CSM velocity, nickel and ejecta masses, and likely low-metallicity environment disfavour a single Wolf-Rayet progenitor star. Instead, a binary companion is likely required to adequately strip the progenitor and produce a low-velocity outflow.

Published
2023

75. A UNIONS view of the brightest central galaxies of candidate fossil groups

Author

Ministerio de Ciencia e Innovación (España), Chu, A., Durret, F., Ellien, A., Sarron, F., Adami, C., Márquez, Isabel, Martinet, N., de Boer, T., Chambers, K. C., Cuillandre, J. -C., Gwyn, S., Magnier, E. A., McConnachie, A. W., Ministerio de Ciencia e Innovación (España), Chu, A., Durret, F., Ellien, A., Sarron, F., Adami, C., Márquez, Isabel, Martinet, N., de Boer, T., Chambers, K. C., Cuillandre, J. -C., Gwyn, S., Magnier, E. A., and McConnachie, A. W.

Abstract

Context. The formation process of fossil groups (FGs) is still under debate, and, because of their relative rarity, large samples of such objects are still missing. Aims. The aim of the present paper is to increase the sample of known FGs, to analyse the properties of their brightest group galaxies (BGGs), and to compare them with a control sample of non-FG BGGs. Methods. We extracted a sample of 87 FG and 100 non-FG candidates from a large spectroscopic catalogue of haloes and galaxies. For all the objects with data available in UNIONS (initially the Canada France Imaging Survey, CFIS) in the u and r bands, and/or in an extra r-band processed to preserve all low-surface-brightness features (rLSB), we performed a 2D photometric fit of the BGG with GALFIT with one or two Sérsic components. We also analysed how the subtraction of the intracluster light (ICL) contribution modifies the BGG properties. From the SDSS spectra available for the BGGs of 65 FGs and 82 non-FGs, we extracted the properties of their stellar populations with Firefly. To complement our study, and in order to provide a detailed illustration of the possible origin of emission lines in the FG BGGs, involving the presence or absence of an AGN, we investigated the origin of the emission lines in a nearby FG that is dominated by the NGC 4104 galaxy. Results. Morphologically, a single Sérsic profile can fit most objects in the u band, while two Sérsics are needed in the r and rLSB bands, both for FGs and non-FGs. Non-FG BGGs cover a larger range of Sérsic index n. FG BGGs follow the Kormendy relation (mean surface brightness versus effective radius) previously derived for almost 1000 brightest cluster galaxies (BCGs), while the majority of non-FGs BGGs are located below this relation, with fainter mean surface brightnesses. This suggests that FG BGGs have evolved similarly to BCGs, and non-FG BGGs have evolved differently from both FG BGGs and BCGs. All the above properties can be strongly modified by th

Published
2023

76. The Optical Light Curve of GRB 221009A:The Afterglow and the Emerging Supernova

Author

Fulton, M. D., Smartt, S. J., Rhodes, L., Huber, M. E., Villar, V. A., Moore, T., Srivastav, S., Schultz, A. S. B., Chambers, K. C., Izzo, L., Hjorth, J., Chen, T.-w., Nicholl, M., Foley, R. J., Rest, A., Smith, K. W., Young, D. R., Sim, S. A., Bright, J., Zenati, Y., De Boer, T., Bulger, J., Fairlamb, J., Gao, H., Lin, C.-c., Lowe, T., Magnier, E. A., Smith, I. A., Wainscoat, R., Coulter, D. A., Jones, D. O., Kilpatrick, C. D., Mcgill, P., Ramirez-ruiz, E., Lee, K.-s., Narayan, G., Ramakrishnan, V., Ridden-harper, R., Singh, A., Wang, Q., Kong, A. K. H., Ngeow, C.-c., Pan, Y.-c., Yang, S., Davis, K. W., Piro, A. L., Rojas-bravo, C., Sommer, J., Yadavalli, S. K., Fulton, M. D., Smartt, S. J., Rhodes, L., Huber, M. E., Villar, V. A., Moore, T., Srivastav, S., Schultz, A. S. B., Chambers, K. C., Izzo, L., Hjorth, J., Chen, T.-w., Nicholl, M., Foley, R. J., Rest, A., Smith, K. W., Young, D. R., Sim, S. A., Bright, J., Zenati, Y., De Boer, T., Bulger, J., Fairlamb, J., Gao, H., Lin, C.-c., Lowe, T., Magnier, E. A., Smith, I. A., Wainscoat, R., Coulter, D. A., Jones, D. O., Kilpatrick, C. D., Mcgill, P., Ramirez-ruiz, E., Lee, K.-s., Narayan, G., Ramakrishnan, V., Ridden-harper, R., Singh, A., Wang, Q., Kong, A. K. H., Ngeow, C.-c., Pan, Y.-c., Yang, S., Davis, K. W., Piro, A. L., Rojas-bravo, C., Sommer, J., and Yadavalli, S. K.

Published
2023

77. Forbidden hugs in pandemic times:IV. Panchromatic evolution of three luminous red novae

Author

Pastorello, A., Valerin, G., Fraser, M., Reguitti, A., Elias-rosa, N., Filippenko, A. V., Rojas-bravo, C., Tartaglia, L., Reynolds, T. M., Valenti, S., Andrews, J. E., Ashall, C., Bostroem, K. A., Brink, T. G., Burke, J., Cai, Y.-z., Cappellaro, E., Coulter, D. A., Dastidar, R., Davis, K. W., Dimitriadis, G., Fiore, A., Foley, R. J., Fugazza, D., Galbany, L., Gangopadhyay, A., Geier, S., Gutiérrez, C. P., Haislip, J., Hiramatsu, D., Holmbo, S., Howell, D. A., Hsiao, E. Y., Hung, T., Jha, S. W., Kankare, E., Karamehmetoglu, E., Kilpatrick, C. D., Kotak, R., Kouprianov, V., Kravtsov, T., Kumar, S., Li, Z.-t., Lundquist, M. J., Lundqvist, P., Matilainen, K., Mazzali, P. A., Mccully, C., Misra, K., Morales-garoffolo, A., Moran, S., Morrell, N., Newsome, M., Padilla Gonzalez, E., Pan, Y.-c., Pellegrino, C., Phillips, M. M., Pignata, G., Piro, A. L., Reichart, D. E., Rest, A., Salmaso, I., Sand, D. J., Siebert, M. R., Smartt, S. J., Smith, K. W., Srivastav, S., Stritzinger, M. D., Taggart, K., Tinyanont, S., Yan, S.-y., Wang, L., Wang, X.-f., Williams, S. C., Wyatt, S., Zhang, T.-m., De Boer, T., Chambers, K., Gao, H., Magnier, E., Pastorello, A., Valerin, G., Fraser, M., Reguitti, A., Elias-rosa, N., Filippenko, A. V., Rojas-bravo, C., Tartaglia, L., Reynolds, T. M., Valenti, S., Andrews, J. E., Ashall, C., Bostroem, K. A., Brink, T. G., Burke, J., Cai, Y.-z., Cappellaro, E., Coulter, D. A., Dastidar, R., Davis, K. W., Dimitriadis, G., Fiore, A., Foley, R. J., Fugazza, D., Galbany, L., Gangopadhyay, A., Geier, S., Gutiérrez, C. P., Haislip, J., Hiramatsu, D., Holmbo, S., Howell, D. A., Hsiao, E. Y., Hung, T., Jha, S. W., Kankare, E., Karamehmetoglu, E., Kilpatrick, C. D., Kotak, R., Kouprianov, V., Kravtsov, T., Kumar, S., Li, Z.-t., Lundquist, M. J., Lundqvist, P., Matilainen, K., Mazzali, P. A., Mccully, C., Misra, K., Morales-garoffolo, A., Moran, S., Morrell, N., Newsome, M., Padilla Gonzalez, E., Pan, Y.-c., Pellegrino, C., Phillips, M. M., Pignata, G., Piro, A. L., Reichart, D. E., Rest, A., Salmaso, I., Sand, D. J., Siebert, M. R., Smartt, S. J., Smith, K. W., Srivastav, S., Stritzinger, M. D., Taggart, K., Tinyanont, S., Yan, S.-y., Wang, L., Wang, X.-f., Williams, S. C., Wyatt, S., Zhang, T.-m., De Boer, T., Chambers, K., Gao, H., and Magnier, E.

Published
2023

78. SN 2023ixf in Messier 101:Photo-ionization of Dense, Close-in Circumstellar Material in a Nearby Type II Supernova

Author

Jacobson-galán, W. V., Dessart, L., Margutti, R., Chornock, R., Foley, R. J., Kilpatrick, C. D., Jones, D. O., Taggart, K., Angus, C. R., Bhattacharjee, S., Braff, L. A., Brethauer, D., Burgasser, A. J., Cao, F., Carlile, C. M., Chambers, K. C., Coulter, D. A., Dominguez-ruiz, E., Dickinson, C. B., De Boer, T., Gagliano, A., Gall, C., Gao, H., Gates, E. L., Gomez, S., Guolo, M., Halford, M. R. J., Hjorth, J., Huber, M. E., Johnson, M. N., Karpoor, P. R., Laskar, T., Lebaron, N, Li, Z., Lin, Y., Loch, S. D., Lynam, P. D., Magnier, E. A., Maloney, P., Matthews, D. J., Mcdonald, M., Miao, H.-y., Milisavljevic, D., Pan, Y.-c., Pradyumna, S., Ransome, C. L., Rees, J. M., Rest, A., Rojas-bravo, C., Sandford, N. R., Ascencio, L. Sandoval, Sanjaripour, S., Savino, A., Sears, H., Sharei, N., Smartt, S. J., Softich, E. R., Theissen, C. A., Tinyanont, S., Tohfa, H., Villar, V. A., Wang, Q., Wainscoat, R. J., Westerling, A. L., Wiston, E., Wozniak, M. A., Yadavalli, S. K., Zenati, Y., Jacobson-galán, W. V., Dessart, L., Margutti, R., Chornock, R., Foley, R. J., Kilpatrick, C. D., Jones, D. O., Taggart, K., Angus, C. R., Bhattacharjee, S., Braff, L. A., Brethauer, D., Burgasser, A. J., Cao, F., Carlile, C. M., Chambers, K. C., Coulter, D. A., Dominguez-ruiz, E., Dickinson, C. B., De Boer, T., Gagliano, A., Gall, C., Gao, H., Gates, E. L., Gomez, S., Guolo, M., Halford, M. R. J., Hjorth, J., Huber, M. E., Johnson, M. N., Karpoor, P. R., Laskar, T., Lebaron, N, Li, Z., Lin, Y., Loch, S. D., Lynam, P. D., Magnier, E. A., Maloney, P., Matthews, D. J., Mcdonald, M., Miao, H.-y., Milisavljevic, D., Pan, Y.-c., Pradyumna, S., Ransome, C. L., Rees, J. M., Rest, A., Rojas-bravo, C., Sandford, N. R., Ascencio, L. Sandoval, Sanjaripour, S., Savino, A., Sears, H., Sharei, N., Smartt, S. J., Softich, E. R., Theissen, C. A., Tinyanont, S., Tohfa, H., Villar, V. A., Wang, Q., Wainscoat, R. J., Westerling, A. L., Wiston, E., Wozniak, M. A., Yadavalli, S. K., and Zenati, Y.

Published
2023

79. The rise and fall of the iron-strong nuclear transient PS16dtm

Author

Petrushevska, T., primary, Leloudas, G., additional, Ilić, D., additional, Bronikowski, M., additional, Charalampopoulos, P., additional, Jaisawal, G. K., additional, Paraskeva, E., additional, Pursiainen, M., additional, Rakić, N., additional, Schulze, S., additional, Taggart, K., additional, Wedderkopp, C. K., additional, Anderson, J. P., additional, de Boer, T., additional, Chambers, K., additional, Chen, T. W., additional, Damljanović, G., additional, Fraser, M., additional, Gao, H., additional, Gomboc, A., additional, Gromadzki, M., additional, Ihanec, N., additional, Maguire, K., additional, Marčun, B., additional, Müller-Bravo, T. E., additional, Nicholl, M., additional, Onori, F., additional, Reynolds, T. M., additional, Smartt, S. J., additional, Sollerman, J., additional, Smith, K. W., additional, Wevers, T., additional, and Wyrzykowski, Ł., additional

Published
2023
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80. A fast-rising tidal disruption event from a candidate intermediate-mass black hole

Author

Angus, C. R., primary, Baldassare, V. F., additional, Mockler, B., additional, Foley, R. J., additional, Ramirez-Ruiz, E., additional, Raimundo, S. I., additional, French, K. D., additional, Auchettl, K., additional, Pfister, H., additional, Gall, C., additional, Hjorth, J., additional, Drout, M. R., additional, Alexander, K. D., additional, Dimitriadis, G., additional, Hung, T., additional, Jones, D. O., additional, Rest, A., additional, Siebert, M. R., additional, Taggart, K., additional, Terreran, G., additional, Tinyanont, S., additional, Carroll, C. M., additional, DeMarchi, L., additional, Earl, N., additional, Gagliano, A., additional, Izzo, L., additional, Villar, V. A., additional, Zenati, Y., additional, Arendse, N., additional, Cold, C., additional, de Boer, T. J. L., additional, Chambers, K. C., additional, Coulter, D. A., additional, Khetan, N., additional, Lin, C. C., additional, Magnier, E. A., additional, Rojas-Bravo, C., additional, Wainscoat, R. J., additional, and Wojtak, R., additional

Published
2022
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81. Forbidden hugs in pandemic times

Author

Cai, Y.-Z., primary, Pastorello, A., additional, Fraser, M., additional, Wang, X.-F., additional, Filippenko, A. V., additional, Reguitti, A., additional, Patra, K. C., additional, Goranskij, V. P., additional, Barsukova, E. A., additional, Brink, T. G., additional, Elias-Rosa, N., additional, Stevance, H. F., additional, Zheng, W., additional, Yang, Y., additional, Atapin, K. E., additional, Benetti, S., additional, de Boer, T. J. L., additional, Bose, S., additional, Burke, J., additional, Byrne, R., additional, Cappellaro, E., additional, Chambers, K. C., additional, Chen, W.-L., additional, Emami, N., additional, Gao, H., additional, Hiramatsu, D., additional, Howell, D. A., additional, Huber, M. E., additional, Kankare, E., additional, Kelly, P. L., additional, Kotak, R., additional, Kravtsov, T., additional, Lander, V. Yu., additional, Li, Z.-T., additional, Lin, C.-C., additional, Lundqvist, P., additional, Magnier, E. A., additional, Malygin, E. A., additional, Maslennikova, N. A., additional, Matilainen, K., additional, Mazzali, P. A., additional, McCully, C., additional, Mo, J., additional, Moran, S., additional, Newsome, M., additional, Oparin, D. V., additional, Padilla Gonzalez, E., additional, Reynolds, T. M., additional, Shatsky, N. I., additional, Smartt, S. J., additional, Smith, K. W., additional, Stritzinger, M. D., additional, Tatarnikov, A. M., additional, Terreran, G., additional, Uklein, R. I., additional, Valerin, G., additional, Vallely, P. J., additional, Vozyakova, O. V., additional, Wainscoat, R., additional, Yan, S.-Y., additional, Zhang, J.-J., additional, Zhang, T.-M., additional, Zheltoukhov, S. G., additional, Dastidar, R., additional, Fulton, M., additional, Galbany, L., additional, Gangopadhyay, A., additional, Ge, H.-W., additional, Gutiérrez, C. P., additional, Lin, H., additional, Misra, K., additional, Ou, Z.-W., additional, Salmaso, I., additional, Tartaglia, L., additional, Xiao, L., additional, and Zhang, X.-H., additional

Published
2022
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82. The nuclear transient AT 2017gge: a tidal disruption event in a dusty and gas-rich environment and the awakening of a dormant SMBH

Author

Onori, F, primary, Cannizzaro, G, additional, Jonker, P G, additional, Kim, M, additional, Nicholl, M, additional, Mattila, S, additional, Reynolds, T M, additional, Fraser, M, additional, Wevers, T, additional, Brocato, E, additional, Anderson, J P, additional, Carini, R, additional, Charalampopoulos, P, additional, Clark, P, additional, Gromadzki, M, additional, Gutiérrez, C P, additional, Ihanec, N, additional, Inserra, C, additional, Lawrence, A, additional, Leloudas, G, additional, Lundqvist, P, additional, Müller-Bravo, T E, additional, Piranomonte, S, additional, Pursiainen, M, additional, Rybicki, K A, additional, Somero, A, additional, Young, D R, additional, Chambers, K C, additional, Gao, H, additional, de Boer, T J L, additional, and Magnier, E A, additional

Published
2022
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83. The Philosophy of Henri Bergson

Author

de Boer, T. J.

Abstract

In 1907, Alfred Binet, as astute a thinker as witty a writer, conducted an inquiry into the state of philosophical education in the French gymnasiums (lycées and collèges) of which he in his Année psychologique (1908) communicates the results. Of the nearly 300 teachers who devote themselves to this teaching, 103 responded to the 18 questions he asked. This relatively large number of answers demonstrates the interest of the respondents in the topic. Are the reliability and, above all, the cor...

Published
2022

84. The Circumstellar Environments of Double-peaked, Calcium-strong Transients 2021gno and 2021inl

Author

Jacobson-Galán, W. V., primary, Venkatraman, P., additional, Margutti, R., additional, Khatami, D., additional, Terreran, G., additional, Foley, R. J., additional, Angulo, R., additional, Angus, C. R., additional, Auchettl, K., additional, Blanchard, P. K., additional, Bobrick, A., additional, Bright, J. S., additional, Brout, D., additional, Chambers, K. C., additional, Couch, C. D., additional, Coulter, D. A., additional, Clever, K., additional, Davis, K. W., additional, de Boer, T. J. L., additional, DeMarchi, L., additional, Dodd, S. A., additional, Jones, D. O., additional, Johnson, J., additional, Kilpatrick, C. D., additional, Khetan, N., additional, Lai, Z., additional, Langeroodi, D., additional, Lin, C.-C., additional, Magnier, E. A., additional, Milisavljevic, D., additional, Perets, H. B., additional, Pierel, J. D. R., additional, Raymond, J., additional, Rest, S., additional, Rest, A., additional, Ridden-Harper, R., additional, Shen, K. J., additional, Siebert, M. R., additional, Smith, C., additional, Taggart, K., additional, Tinyanont, S., additional, Valdes, F., additional, Villar, V. A., additional, Wang, Q., additional, Yadavalli, S. K., additional, Zenati, Y., additional, and Zenteno, A., additional

Published
2022
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86. Forbidden hugs in pandemic times III. Observations of the luminous red nova AT 2021biy in the nearby galaxy NGC 4631

Author

Cai, Y-Z, Pastorello, A., Fraser, M., Wang, X-F, Filippenko, A., Reguitti, A., Patra, K. C., Goranskij, V. P., Barsukova, E. A., Brink, T. G., Elias-Rosa, N., Stevance, H. F., Zheng, W., Yang, Y., Atapin, K. E., Benetti, S., de Boer, T. J. L., Bose, S., Burke, J., Byrne, R., Cappellaro, E., Chambers, K. C., Chen, W-L, Emami, N., Gao, H., Hiramatsu, D., Howell, D. A., Huber, M. E., Kankare, E., Kelly, P. L., Kotak, R., Kravtsov, T., Lander, V. Yu, Li, Z-T, Lin, C-C, Lundqvist, P., Magnier, E. A., Malygin, E. A., Maslennikova, N. A., Matilainen, K., Mazzali, P. A., McCully, C., Mo, J., Moran, S., Newsome, M., Oparin, D., Gonzalez, E. Padilla, Reynolds, T. M., Shatsky, N., Smartt, S. J., Smith, K. W., Stritzinger, M. D., Tatarnikov, A. M., Terreran, G., Uklein, R., Valerin, G., Vallely, P. J., Vozyakova, O. V., Wainscoat, R., Yan, S-Y, Zhang, J-J, Zhang, T-M, Zheltoukhov, S. G., Dastidar, R., Fulton, M., Galbany, L., Gangopadhyay, A., Ge, H-W, Gutierrez, C. P., Lin, H., Misra, K., Ou, Z-W, Salmaso, Nico, Tartaglia, L., Xiao, L., Zhang, X-H, Cai, Y-Z, Pastorello, A., Fraser, M., Wang, X-F, Filippenko, A., Reguitti, A., Patra, K. C., Goranskij, V. P., Barsukova, E. A., Brink, T. G., Elias-Rosa, N., Stevance, H. F., Zheng, W., Yang, Y., Atapin, K. E., Benetti, S., de Boer, T. J. L., Bose, S., Burke, J., Byrne, R., Cappellaro, E., Chambers, K. C., Chen, W-L, Emami, N., Gao, H., Hiramatsu, D., Howell, D. A., Huber, M. E., Kankare, E., Kelly, P. L., Kotak, R., Kravtsov, T., Lander, V. Yu, Li, Z-T, Lin, C-C, Lundqvist, P., Magnier, E. A., Malygin, E. A., Maslennikova, N. A., Matilainen, K., Mazzali, P. A., McCully, C., Mo, J., Moran, S., Newsome, M., Oparin, D., Gonzalez, E. Padilla, Reynolds, T. M., Shatsky, N., Smartt, S. J., Smith, K. W., Stritzinger, M. D., Tatarnikov, A. M., Terreran, G., Uklein, R., Valerin, G., Vallely, P. J., Vozyakova, O. V., Wainscoat, R., Yan, S-Y, Zhang, J-J, Zhang, T-M, Zheltoukhov, S. G., Dastidar, R., Fulton, M., Galbany, L., Gangopadhyay, A., Ge, H-W, Gutierrez, C. P., Lin, H., Misra, K., Ou, Z-W, Salmaso, Nico, Tartaglia, L., Xiao, L., and Zhang, X-H

Abstract

We present an observational study of the luminous red nova (LRN) AT 2021biy in the nearby galaxy NGC 4631. The field of the object was routinely imaged during the pre-eruptive stage by synoptic surveys, but the transient was detected only at a few epochs from similar to 231 days before maximum brightness. The LRN outburst was monitored with unprecedented cadence both photometrically and spectroscopically. AT 2021biy shows a short-duration blue peak, with a bolometric luminosity of similar to 1.6 x 10(41) erg s(-1), followed by the longest plateau among LRNe to date, with a duration of 210 days. A late-time hump in the light curve was also observed, possibly produced by a shell-shell collision. AT 2021biy exhibits the typical spectral evolution of LRNe. Early-time spectra are characterised by a blue continuum and prominent H emission lines. Then, the continuum becomes redder, resembling that of a K-type star with a forest of metal absorption lines during the plateau phase. Finally, late-time spectra show a very red continuum (T-BB approximate to 2050 K) with molecular features (e.g., TiO) resembling those of M-type stars. Spectropolarimetric analysis indicates that AT 2021biy has local dust properties similar to those of V838 Mon in the Milky Way Galaxy. Inspection of archival Hubble Space Telescope data taken on 2003 August 3 reveals a similar to 20 M-circle dot progenitor candidate with log (L/L-circle dot)= 5.0 dex and T-eff = 5900 K at solar metallicity. The above luminosity and colour match those of a luminous yellow supergiant. Most likely, this source is a close binary, with a 17-24 M(circle dot)( )primary component.

Published
2022

87. The nuclear transient AT 2017gge:a tidal disruption event in a dusty and gas-rich environment and the awakening of a dormant SMBH

Author

Onori, F., Cannizzaro, G., Jonker, P. G., Kim, M., Nicholl, M., Mattila, S., Reynolds, T. M., Fraser, M., Wevers, T., Brocato, E., Anderson, J. P., Carini, R., Charalampopoulos, P., Clark, P., Gromadzki, M., Gutierrez, C. P., Ihanec, N., Inserra, C., Lawrence, A., Leloudas, G., Lundqvist, P., Muller-Bravo, T. E., Piranomonte, S., Pursiainen, M., Rybicki, K. A., Somero, A., Young, D. R., Chambers, K. C., Gao, H., de Boer, T. J. L., Magnier, E. A., Onori, F., Cannizzaro, G., Jonker, P. G., Kim, M., Nicholl, M., Mattila, S., Reynolds, T. M., Fraser, M., Wevers, T., Brocato, E., Anderson, J. P., Carini, R., Charalampopoulos, P., Clark, P., Gromadzki, M., Gutierrez, C. P., Ihanec, N., Inserra, C., Lawrence, A., Leloudas, G., Lundqvist, P., Muller-Bravo, T. E., Piranomonte, S., Pursiainen, M., Rybicki, K. A., Somero, A., Young, D. R., Chambers, K. C., Gao, H., de Boer, T. J. L., and Magnier, E. A.

Abstract

We present the results from a dense multwavelength [optical/UV, near-infrared (IR), and X-ray] follow-up campaign of the nuclear transient AT 2017gge, covering a total of 1698 d from the transient's discovery. The bolometric light curve, the blackbody temperature and radius, the broad H and He i lambda 5876 emission lines and their evolution with time, are all consistent with a tidal disruption event (TDE) nature. A soft X-ray flare is detected with a delay of similar to 200 d with respect to the optical/UV peak and it is rapidly followed by the emergence of a broad He ii lambda 4686 and by a number of long-lasting high ionization coronal emission lines. This indicate a clear connection between a TDE flare and the appearance of extreme coronal line emission (ECLEs). An IR echo, resulting from dust re-radiation of the optical/UV TDE light is observed after the X-ray flare and the associated near-IR spectra show a transient broad feature in correspondence of the He i lambda 10830 and, for the first time in a TDE, a transient high-ionization coronal NIR line (the [Fe xiii] lambda 10798) is also detected. The data are well explained by a scenario in which a TDE occurs in a gas-and-dust rich environment and its optical/UV, soft X-ray, and IR emission have different origins and locations. The optical emission may be produced by stellar debris stream collisions prior to the accretion disc formation, which is instead responsible for the soft X-ray flare, emitted after the end of the circularization process.

Published
2022

88. The Circumstellar Environments of Double-peaked, Calcium-strong Transients 2021gno and 2021inl

Author

Jacobson-Galan, W. V., Venkatraman, P., Margutti, R., Khatami, D., Terreran, G., Foley, R. J., Angulo, R., Angus, C. R., Auchettl, K., Blanchard, P. K., Bobrick, A., Bright, J. S., Brout, D., Chambers, K. C., Couch, C. D., Coulter, D. A., Clever, K., Davis, K. W., de Boer, T. J. L., DeMarchi, L., Dodd, S. A., Jones, D. O., Johnson, J., Kilpatrick, C. D., Khetan, N., Lai, Z., Langeroodi, D., Lin, C. -C., Magnier, E. A., Milisavljevic, D., Perets, H. B., Pierel, J. D. R., Raymond, J., Rest, S., Rest, A., Ridden-Harper, R., Shen, K. J., Siebert, M. R., Smith, C., Taggart, K., Tinyanont, S., Valdes, F., Villar, V. A., Wang, Q., Yadavalli, S. K., Zenati, Y., Zenteno, A., Jacobson-Galan, W. V., Venkatraman, P., Margutti, R., Khatami, D., Terreran, G., Foley, R. J., Angulo, R., Angus, C. R., Auchettl, K., Blanchard, P. K., Bobrick, A., Bright, J. S., Brout, D., Chambers, K. C., Couch, C. D., Coulter, D. A., Clever, K., Davis, K. W., de Boer, T. J. L., DeMarchi, L., Dodd, S. A., Jones, D. O., Johnson, J., Kilpatrick, C. D., Khetan, N., Lai, Z., Langeroodi, D., Lin, C. -C., Magnier, E. A., Milisavljevic, D., Perets, H. B., Pierel, J. D. R., Raymond, J., Rest, S., Rest, A., Ridden-Harper, R., Shen, K. J., Siebert, M. R., Smith, C., Taggart, K., Tinyanont, S., Valdes, F., Villar, V. A., Wang, Q., Yadavalli, S. K., Zenati, Y., and Zenteno, A.

Abstract

We present panchromatic observations and modeling of calcium-strong supernovae (SNe) 2021gno in the star-forming host-galaxy NGC 4165 and 2021inl in the outskirts of elliptical galaxy NGC 4923, both monitored through the Young Supernova Experiment transient survey. The light curves of both, SNe show two peaks, the former peak being derived from shock cooling emission (SCE) and/or shock interaction with circumstellar material (CSM). The primary peak in SN 2021gno is coincident with luminous, rapidly decaying X-ray emission (L-x = 5 x 10(41) erg s(-1)) detected by Swift-XRT at delta t = 1 day after explosion, this observation being the second-ever detection of X-rays from a calcium-strong transient. We interpret the X-ray emission in the context of shock interaction with CSM that extends to r < 3 x 10(14) cm. Based on X-ray modeling, we calculate a CSM mass M-CSM = (0.3-1.6) x 10(-3) M-circle dot and density n = (1-4) x 10(10) cm(-3). Radio nondetections indicate a low-density environment at larger radii (r > 10(16) cm) and mass-loss rate of M < 10(-4) M-circle dot yr(-1). SCE modeling of both primary light-curve peaks indicates an extended-progenitor envelope mass M-e = 0.02-0.05 M-circle dot and radius R-e = 30-230 R-circle dot. The explosion properties suggest progenitor systems containing either a low-mass massive star or a white dwarf (WD), the former being unlikely given the lack of local star formation. Furthermore, the environments of both SNe are consistent with low-mass hybrid He/C/O WD + C/O WD mergers.

Published
2022

89. Final Moments. I. Precursor Emission, Envelope Inflation, and Enhanced Mass Loss Preceding the Luminous Type II Supernova 2020tlf

Author

Jacobson-galán, W. V., Dessart, L., Jones, D. O., Margutti, R., Coppejans, D. L., Dimitriadis, G., Foley, R. J., Kilpatrick, C. D., Matthews, D. J., Rest, S., Terreran, G., Aleo, P. D., Auchettl, K., Blanchard, P. K., Coulter, D. A., Davis, K. W., De Boer, T. J. L., Demarchi, L., Drout, M. R., Earl, N., Gagliano, A., Gall, C., Hjorth, J., Huber, M. E., Ibik, A. L., Milisavljevic, D., Pan, Y.-c., Rest, A., Ridden-harper, R., Rojas-bravo, C., Siebert, M. R., Smith, K. W., Taggart, K., Tinyanont, S., Wang, Q., Zenati, Y., Jacobson-galán, W. V., Dessart, L., Jones, D. O., Margutti, R., Coppejans, D. L., Dimitriadis, G., Foley, R. J., Kilpatrick, C. D., Matthews, D. J., Rest, S., Terreran, G., Aleo, P. D., Auchettl, K., Blanchard, P. K., Coulter, D. A., Davis, K. W., De Boer, T. J. L., Demarchi, L., Drout, M. R., Earl, N., Gagliano, A., Gall, C., Hjorth, J., Huber, M. E., Ibik, A. L., Milisavljevic, D., Pan, Y.-c., Rest, A., Ridden-harper, R., Rojas-bravo, C., Siebert, M. R., Smith, K. W., Taggart, K., Tinyanont, S., Wang, Q., and Zenati, Y.

Published
2022

90. SN 2020kyg and the rates of faint Iax supernovae from ATLAS

Author

Srivastav, Shubham, Smartt, S. J., Huber, M. E., Chambers, K. C., Angus, C. R., Chen, T-W, Callan, F. P., Gillanders, J. H., McBrien, O. R., Sim, S. A., Fulton, M., Hjorth, J., Smith, K. W., Young, D. R., Auchettl, K., Anderson, J. P., Pignata, G., de Boer, T. J. L., Lin, C-C, Magnier, E. A., Srivastav, Shubham, Smartt, S. J., Huber, M. E., Chambers, K. C., Angus, C. R., Chen, T-W, Callan, F. P., Gillanders, J. H., McBrien, O. R., Sim, S. A., Fulton, M., Hjorth, J., Smith, K. W., Young, D. R., Auchettl, K., Anderson, J. P., Pignata, G., de Boer, T. J. L., Lin, C-C, and Magnier, E. A.

Abstract

We present multiwavelength follow-up observations of the ATLAS discovered faint Iax supernova SN 2020kyg that peaked at an absolute magnitude of M-g approximate to -14.9 +/- 0.2, making it another member of the faint Iax supernova population. The bolometric light curve requires only approximate to 7 x 10(-3) M-circle dot of radioactive Ni-56, with an ejected mass of M-ej similar to 0.4 M-circle dot and a low kinetic energy of E approximate to 0.05 +/- 0.02 x 10(51) erg. We construct a homogeneous volume-limited sample of 902 transients observed by ATLAS within 100 Mpc during a 3.5 yr span. Using this sample, we constrain the rates of faint Iax (M-r greater than or similar to -16) events within 60 Mpc at 12(-8)(+1)(4) per cent of the SN Ia rate. The overall Iax rate, at 15(-9)(+)(17) per cent of the Ia rate, is dominated by the low-luminosity events, with luminous SNe Iax (M-r less than or similar to -17.5) like 2002cx and 2005hk, accounting for only 0.9(-0.5)(+1.1) per cent of the Ia rate (a 2 sigma upper limit of approximately 3 per cent). We favour the hybrid CONe WD + He star progenitor channel involving a failed deflagration of a near Chandrasekhar mass white dwarf, expected to leave a bound remnant and a surviving secondary companion, as a candidate explanation for faint Iax explosions. This scenario requires short delay times, consistent with the observed environments of SNe Iax. Furthermore, binary population synthesis calculations have suggested rates of 1-18 per cent of the SN Ia rate for this channel, consistent with our rate estimates.

Published
2022

91. The synchronized dance of the magellanic clouds’ star formation history

Author

Massana, P, primary, Ruiz-Lara, T, additional, Noël, N E D, additional, Gallart, C, additional, Nidever, D L, additional, Choi, Y, additional, Sakowska, J D, additional, Besla, G, additional, Olsen, K A G, additional, Monelli, M, additional, Dorta, A, additional, Stringfellow, G S, additional, Cassisi, S, additional, Bernard, E J, additional, Zaritsky, D, additional, Cioni, M-R L, additional, Monachesi, A, additional, van der Marel, R P, additional, de Boer, T J L, additional, and Walker, A R, additional

Published
2022
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93. SN 2020kyg and the rates of faint Iax supernovae from ATLAS

Author

Srivastav, Shubham, primary, Smartt, S J, additional, Huber, M E, additional, Chambers, K C, additional, Angus, C R, additional, Chen, T-W, additional, Callan, F P, additional, Gillanders, J H, additional, McBrien, O R, additional, Sim, S A, additional, Fulton, M, additional, Hjorth, J, additional, Smith, K W, additional, Young, D R, additional, Auchettl, K, additional, Anderson, J P, additional, Pignata, G, additional, de Boer, T J L, additional, Lin, C-C, additional, and Magnier, E A, additional

Published
2022
Full Text
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94. Final Moments. I. Precursor Emission, Envelope Inflation, and Enhanced Mass Loss Preceding the Luminous Type II Supernova 2020tlf

Author

Jacobson-Galán, W. V., primary, Dessart, L., additional, Jones, D. O., additional, Margutti, R., additional, Coppejans, D. L., additional, Dimitriadis, G., additional, Foley, R. J., additional, Kilpatrick, C. D., additional, Matthews, D. J., additional, Rest, S., additional, Terreran, G., additional, Aleo, P. D., additional, Auchettl, K., additional, Blanchard, P. K., additional, Coulter, D. A., additional, Davis, K. W., additional, de Boer, T. J. L., additional, DeMarchi, L., additional, Drout, M. R., additional, Earl, N., additional, Gagliano, A., additional, Gall, C., additional, Hjorth, J., additional, Huber, M. E., additional, Ibik, A. L., additional, Milisavljevic, D., additional, Pan, Y.-C., additional, Rest, A., additional, Ridden-Harper, R., additional, Rojas-Bravo, C., additional, Siebert, M. R., additional, Smith, K. W., additional, Taggart, K., additional, Tinyanont, S., additional, Wang, Q., additional, and Zenati, Y., additional

Published
2022
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96. The DECam Local Volume Exploration Survey: Overview and First Data Release

Author

Drlica-Wagner, A., primary, Carlin, J. L., additional, Nidever, D. L., additional, Ferguson, P. S., additional, Kuropatkin, N., additional, Adamów, M., additional, Cerny, W., additional, Choi, Y., additional, Esteves, J. H., additional, Martínez-Vázquez, C. E., additional, Mau, S., additional, Miller, A. E., additional, Mutlu-Pakdil, B., additional, Neilsen, E. H., additional, Olsen, K. A. G., additional, Pace, A. B., additional, Riley, A. H., additional, Sakowska, J. D., additional, Sand, D. J., additional, Santana-Silva, L., additional, Tollerud, E. J., additional, Tucker, D. L., additional, Vivas, A. K., additional, Zaborowski, E., additional, Zenteno, A., additional, Abbott, T. M. C., additional, Allam, S., additional, Bechtol, K., additional, Bell, C. P. M., additional, Bell, E. F., additional, Bilaji, P., additional, Bom, C. R., additional, Carballo-Bello, J. A., additional, Crnojević, D., additional, Cioni, M.-R. L., additional, Diaz-Ocampo, A., additional, de Boer, T. J. L., additional, Erkal, D., additional, Gruendl, R. A., additional, Hernandez-Lang, D., additional, Hughes, A. K., additional, James, D. J., additional, Johnson, L. C., additional, Li, T. S., additional, Mao, Y.-Y., additional, Martínez-Delgado, D., additional, Massana, P., additional, McNanna, M., additional, Morgan, R., additional, Nadler, E. O., additional, Noël, N. E. D., additional, Palmese, A., additional, Peter, A. H. G., additional, Rykoff, E. S., additional, Sánchez, J., additional, Shipp, N., additional, Simon, J. D., additional, Smercina, A., additional, Soares-Santos, M., additional, Stringfellow, G. S., additional, Tavangar, K., additional, van der Marel, R. P., additional, Walker, A. R., additional, Wechsler, R. H., additional, Wu, J. F., additional, Yanny, B., additional, Fitzpatrick, M., additional, Huang, L., additional, Jacques, A., additional, Nikutta, R., additional, and Scott, A., additional

Published
2021
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98. Immunophenotyping Reveals Longitudinal Changes in Circulating Immune Cells During Radium-223 Therapy in Patients With Metastatic Castration-Resistant Prostate Cancer

Author

Creemers, J.H.A., Doelen, M.J. van der, Wilpe, S. van, Hermsen, Rick, Duiveman-de Boer, T., Somford, Diederik M., Janssen, M.J.R., Mehra, N., Textor, J.C., Westdorp, H., Creemers, J.H.A., Doelen, M.J. van der, Wilpe, S. van, Hermsen, Rick, Duiveman-de Boer, T., Somford, Diederik M., Janssen, M.J.R., Mehra, N., Textor, J.C., and Westdorp, H.

Abstract

Contains fulltext : 233864.pdf (Publisher’s version ) (Open Access)

Published
2021

99. Whole Blood Transcriptome Profiling Identifies DNA Replication and Cell Cycle Regulation as Early Marker of Response to Anti-PD-1 in Patients with Urothelial Cancer

Author

Wilpe, S. van, Wosika, V., Ciarloni, L., Ehrensberger, S.H., Jeitziner, R., Angelino, P., Duiveman-de Boer, T., Koornstra, R.H., Vries, I.J.M. de, Gerritsen, W.R., Schalken, J.A., Mehra, N., Wilpe, S. van, Wosika, V., Ciarloni, L., Ehrensberger, S.H., Jeitziner, R., Angelino, P., Duiveman-de Boer, T., Koornstra, R.H., Vries, I.J.M. de, Gerritsen, W.R., Schalken, J.A., and Mehra, N.

Abstract

Contains fulltext : 237712.pdf (Publisher’s version ) (Open Access), Although immune checkpoint inhibitors improve median overall survival in patients with metastatic urothelial cancer (mUC), only a minority of patients benefit from it. Early blood-based response biomarkers may provide a reliable way to assess response weeks before imaging is available, enabling an early switch to other therapies. We conducted an exploratory study aimed at the identification of early markers of response to anti-PD-1 in patients with mUC. Whole blood RNA sequencing and phenotyping of peripheral blood mononuclear cells were performed on samples of 26 patients obtained before and after 2 to 6 weeks of anti-PD-1. Between baseline and on-treatment samples of patients with clinical benefit, 51 differentially expressed genes (DEGs) were identified, of which 37 were upregulated during treatment. Among the upregulated genes was PDCD1, the gene encoding PD-1. STRING network analysis revealed a cluster of five interconnected DEGs which were all involved in DNA replication or cell cycle regulation. We hypothesized that the upregulation of DNA replication/cell cycle genes is a result of T cell proliferation and we were able to detect an increase in Ki-67(+) CD8(+) T cells in patients with clinical benefit (median increase: 1.65%, range -0.63 to 7.06%, p = 0.012). In patients without clinical benefit, no DEGs were identified and no increase in Ki-67(+) CD8(+) T cells was observed. In conclusion, whole blood transcriptome profiling identified early changes in DNA replication and cell cycle regulation genes as markers of clinical benefit to anti-PD-1 in patients with urothelial cancer. Although promising, our findings require further validation before implementation in the clinic.

Published
2021

100. Istaroxime treatment ameliorates calcium dysregulation in a zebrafish model of phospholamban R14del cardiomyopathy

Author

Kamel, S M, van Opbergen, C J M, Koopman, C D, Verkerk, A O, Boukens, B J D, de Jonge, B, Onderwater, Y L, van Alebeek, E, Chocron, S, Polidoro Pontalti, C, Weuring, W J, Vos, M A, de Boer, T P, van Veen, T A B, Bakkers, J, Kamel, S M, van Opbergen, C J M, Koopman, C D, Verkerk, A O, Boukens, B J D, de Jonge, B, Onderwater, Y L, van Alebeek, E, Chocron, S, Polidoro Pontalti, C, Weuring, W J, Vos, M A, de Boer, T P, van Veen, T A B, and Bakkers, J

Abstract

The heterozygous Phospholamban p.Arg14del mutation is found in patients with dilated or arrhythmogenic cardiomyopathy. This mutation triggers cardiac contractile dysfunction and arrhythmogenesis by affecting intracellular Ca2+ dynamics. Little is known about the physiological processes preceding induced cardiomyopathy, which is characterized by sub-epicardial accumulation of fibrofatty tissue, and a specific drug treatment is currently lacking. Here, we address these issues using a knock-in Phospholamban p.Arg14del zebrafish model. Hearts from adult zebrafish with this mutation display age-related remodeling with sub-epicardial inflammation and fibrosis. Echocardiography reveals contractile variations before overt structural changes occur, which correlates at the cellular level with action potential duration alternans. These functional alterations are preceded by diminished Ca2+ transient amplitudes in embryonic hearts as well as an increase in diastolic Ca2+ level, slower Ca2+ transient decay and longer Ca2+ transients in cells of adult hearts. We find that istaroxime treatment ameliorates the in vivo Ca2+ dysregulation, rescues the cellular action potential duration alternans, while it improves cardiac relaxation. Thus, we present insight into the pathophysiology of Phospholamban p.Arg14del cardiomyopathy.

Published
2021

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