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1. Procesado electroquímico de un polímero conductor: mimetismo con los metales

Author

Villanueva, S., Otero, T. F., Brillas, E., and Carrasco, J.

Subjects
Electrogeneration, electrodissolution, electrodeposition, soluble conducting polymers, Electrogeneración, electrodisolución, electrodepósito, polímeros conductores solubles, Clay industries. Ceramics. Glass, TP785-869
Abstract

When an anodic current density of 0.5 mA. cm-2 is applied during 60 s through acetonitrile solutions containing, 5 mM SNS + 0.1 M LiClO4, adherent and uniform poly(SNS) films are electrogenerated on a platinum electrode. These polymeric films can be electrodissolved in the background solution when a cathodic current density is applied. They can be also electrodeposited from solutions of the reduced polymer in the background solution by flow of an anodic current. In this work the influence of different electrolytes: tetraethylammonium perchlorate (TEAClO4), tetrabutylammonium perchlorate (TBAClO4) and tetrahexyl-ammonium perchlorate (THAClO4) in electrogeneration, electrodissolution and electro deposition processes has been studied.Se ha demostrado que aplicando una densidad de corriente anódica de 0.5 mA. cm-2 a través de una disolución de acetonitrilo de concentración 5 mM en SNS y 0.1 M en LiClO4, se obtienen películas de poli(SNS) adherentes y uniformes sobre un electrodo de platino. Estas películas poliméricas pueden electrodisolverse (al aplicar una densidad de corriente catódica) y electrodepositarse (al oxidar las cadenas poliméricas que se encuentran reducidas y disueltas en la disolución de fondo). En este trabajo se ha estudiado la influencia de distintos electrolitos: tetraetilamonioperclorato (TEAClO4), tetrabutilamonioperclorato (TBAClO4) y tetrahexilamonioperclorato (THAClO4) en los procesos de electrogeneración, electrodisolución y electrodepósito.

Published
2000

2. Two long-period transiting exoplanets on eccentric orbits: NGTS-20 b (TOI-5152 b) and TOI-5153 b

Author

Ulmer-Moll, S., Lendl, M., Gill, S., Villanueva, S., Hobson, M. J., Bouchy, F., Brahm, R., Dragomir, D., Grieves, N., Mordasini, C., Anderson, D. R., Acton, J. S., Bayliss, D., Bieryla, A., Burleigh, M. R., Casewell, S. L., Chaverot, G., Eigmüller, P., Feliz, D., Gaudi, S., Gillen, E., Goad, M. R., Gupta, A. F., Günther, M. N., Henderson, B. A., Henning, T., Jenkins, J. S., Jones, M., Jordán, A., Kendall, A., Latham, D. W., Mireles, I., Moyano, M., Nadol, J., Osborn, H. P., Pepper, J., Pinto, M. T., Psaridi, A., Queloz, D., Quinn, S., Rojas, F., Sarkis, P., Schlecker, M., Tilbrook, R. H., Torres, P., Trifonov, T., Udry, S., Vines, J. I., West, R., Wheatley, P., Yao, X., Zhao, Y., and Zhou, G.

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

Long-period transiting planets provide the opportunity to better understand the formation and evolution of planetary systems. Their atmospheric properties remain largely unaltered by tidal or radiative effects of the host star, and their orbital arrangement reflects a different, and less extreme, migrational history compared to close-in objects. The sample of long-period exoplanets with well determined masses and radii is still limited, but a growing number of long-period objects reveal themselves in the TESS data. Our goal is to vet and confirm single transit planet candidates detected in the TESS space-based photometric data through spectroscopic and photometric follow up observations with ground-based instruments. We use the Next Generation Transit Survey (NGTS) to photometrically monitor the candidates in order to observe additional transits. We report the discovery of two massive, warm Jupiter-size planets, one orbiting the F8-type star TOI-5153 and the other orbiting the G1-type star NGTS-20 (=TOI-5152). From our spectroscopic analysis, both stars are metal-rich with a metallicity of 0.12 and 0.15, respectively. Follow-up radial velocity observations were carried out with CORALIE, CHIRON, FEROS, and HARPS. TOI-5153 hosts a 20.33 day period planet with a planetary mass of 3.26 (+-0.18) Mj, a radius of 1.06 (+-0.04) Rj , and an orbital eccentricity of 0.091 (+-0.026). NGTS-20 b is a 2.98 (+-0.16) Mj planet with a radius of 1.07 (+-0.04) Rj on an eccentric (0.432 +- 0.023) orbit with an orbital period of 54.19 days. Both planets are metal-enriched and their heavy element content is in line with the previously reported mass-metallicity relation for gas giants. Both warm Jupiters orbit moderately bright host stars making these objects valuable targets for follow-up studies of the planetary atmosphere and measurement of the spin-orbit angle of the system., Comment: 17 pages, 13 figures, accepted to A&A

Published
2022
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4. The TOI-763 system: sub-Neptunes orbiting a Sun-like star

Author

Fridlund, M., Livingston, J., Gandolfi, D., Persson, C. M., Lam, K. W. F., Stassun, K. G., Hellier, C., Korth, J., Hatzes, A. P., Malavolta, L., Luque, R., Redfield, S., Guenther, E. W., Albrecht, S., Barragan, O., Benatti, S., Bouma, L., Cabrera, J., Cochran, W. D., Csizmadia, Sz., Dai, F., Deeg, H. J., Esposito, M., Georgieva, I., Grziwa, S., Cuesta, L. González, Hirano, T., Jenkins, J. M., Kabath, P., Knudstrup, E., Latham, D. W., Mathur, S., Mullally, S. E., Narita, N., Nowak, G., Olofsson, A. O. H., Palle, E., Pätzold, M., Pompei, E., Rauer, H., Ricker, G., Rodler, F., Seager, S., Serrano, L. M., Smith, A. M. S., Spina, L., Subjak, J., Tenenbaum, P., Ting, E. B., Vanderburg, A., Vanderspek, R., Van Eylen, V., Villanueva, S., and Winn, J. N.

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

We report the discovery of a planetary system orbiting TOI-763 (aka CD-39 7945), a $V=10.2$, high proper motion G-type dwarf star that was photometrically monitored by the TESS space mission in Sector 10. We obtain and model the stellar spectrum and find an object slightly smaller than the Sun, and somewhat older, but with a similar metallicity. Two planet candidates were found in the light curve to be transiting the star. Combining TESS transit photometry with HARPS high-precision radial velocity follow-up measurements confirm the planetary nature of these transit signals. We determine masses, radii, and bulk densities of these two planets. A third planet candidate was discovered serendipitously in the radial velocity data. The inner transiting planet,TOI-763 b, has an orbital period of $P_\mathrm{b}$ = 5.6~days, a mass of $M_\mathrm{b}$ = $9.8\pm0.8$ $M_\oplus$, and a radius of $R_\mathrm{b}$ = $2.37\pm0.10$ $R_\oplus$. The second transiting planet,TOI-763 c, has an orbital period of $P_\mathrm{c}$ = 12.3~days, a mass of $M_\mathrm{c}$ = $9.3\pm1.0$ $M_\oplus$, and a radius of $R_\mathrm{c}$ = $2.87\pm0.11$ $R_\oplus$. We find the outermost planet candidate to orbit the star with a period of $\sim$48~days. If confirmed as a planet it would have a minimum mass of $M_\mathrm{d}$ = $9.5\pm1.6$ $M_\oplus$. We investigated the TESS light curve in order to search for a mono transit by planet~d without success. We discuss the importance and implications of this planetary system in terms of the geometrical arrangements of planets orbiting G-type stars.

Published
2020
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6. Two new HATNet hot Jupiters around A stars, and the first glimpse at the occurrence rate of hot Jupiters from TESS

Author

Zhou, G., Huang, C. X., Bakos, G. Á., Hartman, J. D., Latham, David W., Quinn, S. N., Collins, K. A., Winn, J. N., Wong, I., Kovács, G., Csubry, Z., Bhatti, W., Penev, K., Bieryla, A., Esquerdo, G. A., Berlind, P., Calkins, M. L., de Val-Borro, M., Noyes, R. W., Lázár, J., Papp, I., Sári, P., Kovács, T., Buchhave, Lars A., Szklenár, T., Beky, B., Johnson, M. C., Cochran, W. D., Kniazev, A. Y., Stassun, K. G., Fulton, B. J., Shporer, A., Espinoza, N., Bayliss, D., Everett, M., Howell, S. B., Hellier, C., Anderson, D. R., Cameron, A. Collier, West, R. G., Brown, D. J. A., Schanche, N., Barkaoui, K., Pozuelos, F., Gillon, M., Jehin, E., Benkhaldoun, Z., Daassou, A., Ricker, G., Vanderspek, R., Seager, S., Jenkins, J. M., Lissauer, Jack J., Armstrong, J. D., Collins, K. I., Gan, T., Hart, R., Horne, K., Kielkopf, J. F., Nielsen, L. D., Nishiumi, T., Narita, N., Palle, E., Relles, H. M., Sefako, R., Tan, T. G., Davies, M., Goeke, Robert F., Guerrero, N., Haworth, K., and Villanueva, S.

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

Wide field surveys for transiting planets are well suited to searching diverse stellar populations, enabling a better understanding of the link between the properties of planets and their parent stars. We report the discovery of HAT-P-69b (TOI 625.01) and HAT-P-70b (TOI 624.01), two new hot Jupiters around A stars from the HATNet survey which have also been observed by the Transiting Exoplanet Survey Satellite (TESS). HAT-P-69b has a mass of 3.58 +0.58/-0.58 MJup and a radius of 1.676 +0.051/-0.033 RJup, residing in a prograde 4.79-day orbit. HAT-P-70b has a radius of 1.87 +0.15/-0.10 RJup and a mass constraint of < 6.78 (3 sigma) MJup, and resides in a retrograde 2.74-day orbit. We use the confirmation of these planets around relatively massive stars as an opportunity to explore the occurrence rate of hot Jupiters as a function of stellar mass. We define a sample of 47,126 main-sequence stars brighter than Tmag=10 that yields 31 giant planet candidates, including 18 confirmed planets, 3 candidates, and 10 false positives. We find a net hot Jupiter occurrence rate of 0.41+/-0.10 % within this sample, consistent with the rate measured by Kepler for FGK stars. When divided into stellar mass bins, we find the occurrence rate to be 0.71+/-0.31% for G stars, 0.43+/-0.15% for F stars, and 0.26+/-0.11% for A stars. Thus, at this point, we cannot discern any statistically significant trend in the occurrence of hot Jupiters with stellar mass., Comment: Accepted for publication by AJ

Published
2019
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7. K2 Observations of SN 2018oh Reveal a Two-component Rising Light Curve for a Type Ia Supernova

Author

Dimitriadis, G, Foley, RJ, Rest, A, Kasen, D, Piro, AL, Polin, A, Jones, DO, Villar, A, Narayan, G, Coulter, DA, Kilpatrick, CD, Pan, Y-C, Rojas-Bravo, C, Fox, OD, Jha, SW, Nugent, PE, Riess, AG, Scolnic, D, Drout, MR, Barentsen, G, Dotson, J, Gully-Santiago, M, Hedges, C, Cody, AM, Barclay, T, Howell, S, Garnavich, P, Tucker, BE, Shaya, E, Mushotzky, R, Olling, RP, Margheim, S, Zenteno, A, Coughlin, J, Van Cleve, JE, de Miranda Cardoso, J Vinícius, Larson, KA, McCalmont-Everton, KM, Peterson, CA, Ross, SE, Reedy, LH, Osborne, D, McGinn, C, Kohnert, L, Migliorini, L, Wheaton, A, Spencer, B, Labonde, C, Castillo, G, Beerman, G, Steward, K, Hanley, M, Larsen, R, Gangopadhyay, R, Kloetzel, R, Weschler, T, Nystrom, V, Moffatt, J, Redick, M, Griest, K, Packard, M, Muszynski, M, Kampmeier, J, Bjella, R, Flynn, S, Elsaesser, B, Chambers, KC, Flewelling, HA, Huber, ME, Magnier, EA, Waters, CZ, Schultz, ASB, Bulger, J, Lowe, TB, Willman, M, Smartt, SJ, Smith, KW, Points, S, Strampelli, GM, Brimacombe, J, Chen, P, Muñoz, JA, Mutel, RL, Shields, J, Vallely, PJ, Villanueva, S, Li, W, Wang, X, Zhang, J, Lin, H, Mo, J, Zhao, X, Sai, H, Zhang, X, Zhang, K, Zhang, T, Wang, L, Baron, E, and DerKacy, JM

Subjects
Astronomical Sciences, Physical Sciences, supernovae: general, supernovae: individual, astro-ph.HE, Astronomical and Space Sciences, Astronomy & Astrophysics, Astronomical sciences, Space sciences
Abstract

We present an exquisite 30 minute cadence Kepler (K2) light curve of the Type Ia supernova (SN Ia) 2018oh (ASASSN-18bt), starting weeks before explosion, covering the moment of explosion and the subsequent rise, and continuing past peak brightness. These data are supplemented by multi-color Panoramic Survey Telescope (Pan-STARRS1) and Rapid Response System 1 and Cerro Tololo Inter-American Observatory 4 m Dark Energy Camera (CTIO 4-m DECam) observations obtained within hours of explosion. The K2 light curve has an unusual two-component shape, where the flux rises with a steep linear gradient for the first few days, followed by a quadratic rise as seen for typical supernovae (SNe) Ia. This "flux excess" relative to canonical SN Ia behavior is confirmed in our i-band light curve, and furthermore, SN 2018oh is especially blue during the early epochs. The flux excess peaks 2.14 ± 0.04 days after explosion, has a FWHM of 3.12 ± 0.04 days, a blackbody temperature of K, a peak luminosity of , and a total integrated energy of . We compare SN 2018oh to several models that may provide additional heating at early times, including collision with a companion and a shallow concentration of radioactive nickel. While all of these models generally reproduce the early K2 light curve shape, we slightly favor a companion interaction, at a distance of ∼ based on our early color measurements, although the exact distance depends on the uncertain viewing angle. Additional confirmation of a companion interaction in future modeling and observations of SN 2018oh would provide strong support for a single-degenerate progenitor system.

Published
2019

8. Velocity-resolved Reverberation Mapping of Five Bright Seyfert 1 Galaxies

Author

De Rosa, G, Fausnaugh, MM, Grier, CJ, Peterson, BM, Denney, KD, Horne, Keith, Bentz, MC, Ciroi, S, Bontà, E Dalla, Joner, MD, Kaspi, S, Kochanek, CS, Pogge, RW, Sergeev, SG, Vestergaard, M, Adams, SM, Antognini, J, Salvo, C Araya, Armstrong, E, Bae, J, Barth, AJ, Beatty, TG, Bhattacharjee, A, Borman, GA, Boroson, TA, Bottorff, MC, Brown, JE, Brown, JS, Brotherton, MS, Coker, CT, Clanton, C, Cracco, V, Crawford, SM, Croxall, KV, Eftekharzadeh, S, Eracleous, M, Fiorenza, SL, Frassati, A, Hawkins, K, Henderson, CB, Holoien, TW-S, Hutchison, T, Kellar, J, Kilerci-Eser, E, Kim, S, King, AL, La Mura, G, Laney, CD, Li, M, Lochhaas, C, Ma, Z, MacInnis, F, Manne-Nicholas, ER, Mason, M, McGraw, SM, Mogren, K, Montouri, C, Moody, JW, Mosquera, AM, Mudd, D, Musso, R, Nazarov, SV, Nguyen, ML, Ochner, P, Okhmat, DN, Onken, CA, Ou-Yang, B, Pancoast, A, Pei, L, Penny, M, Poleski, R, Portaluri, E, Prieto, J-L, Price-Whelan, AM, Pulatova, NG, Rafter, S, Roettenbacher, RM, Romero-Colmenero, E, Runnoe, J, Schimoia, JS, Shappee, BJ, Sherf, N, Simonian, GV, Siviero, A, Skowron, DM, Skowron, J, Somers, G, Spencer, M, Starkey, DA, Stevens, DJ, Stoll, R, Tamajo, E, Tayar, J, van Saders, JL, Valenti, S, Villanueva, S, Villforth, C, Weiss, Y, Winkler, H, and Zastrow, J

Subjects
galaxies: active, galaxies: nuclei, galaxies: Seyfert, astro-ph.GA, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry (incl. Structural), Astronomy & Astrophysics
Abstract

We present the first results from a reverberation-mapping campaign undertaken during the first half of 2012, with additional data on one active galactic nucleus (AGN) (NGC 3227) from a 2014 campaign. Our main goals are (1) to determine the black hole masses from continuum-Hβ reverberation signatures, and (2) to look for velocity-dependent time delays that might be indicators of the gross kinematics of the broad-line region. We successfully measure Hβ time delays and black hole masses for five AGNs, four of which have previous reverberation mass measurements. The values measured here are in agreement with earlier estimates, though there is some intrinsic scatter beyond the formal measurement errors. We observe velocity-dependent Hβ lags in each case, and find that the patterns have changed in the intervening five years for three AGNs that were also observed in 2007.

Published
2018

9. Continuum Reverberation Mapping of the Accretion Disks in Two Seyfert 1 Galaxies

Author

Fausnaugh, MM, Starkey, DA, Horne, Keith, Kochanek, CS, Peterson, BM, Bentz, MC, Denney, KD, Grier, CJ, Grupe, D, Pogge, RW, De Rosa, G, Adams, SM, Barth, AJ, Beatty, Thomas G, Bhattacharjee, A, Borman, GA, Boroson, TA, Bottorff, MC, Brown, Jacob E, Brown, Jonathan S, Brotherton, MS, Coker, CT, Crawford, SM, Croxall, KV, Eftekharzadeh, Sarah, Eracleous, Michael, Joner, MD, Henderson, CB, Holoien, TW-S, Hutchison, T, Kaspi, Shai, Kim, S, King, Anthea L, Li, Miao, Lochhaas, Cassandra, Ma, Zhiyuan, MacInnis, F, Manne-Nicholas, ER, Mason, M, Montuori, Carmen, Mosquera, Ana, Mudd, Dale, Musso, R, Nazarov, SV, Nguyen, ML, Okhmat, DN, Onken, Christopher A, Ou-Yang, B, Pancoast, A, Pei, L, Penny, Matthew T, Poleski, Radosław, Rafter, Stephen, Romero-Colmenero, E, Runnoe, Jessie, Sand, David J, Schimoia, Jaderson S, Sergeev, SG, Shappee, BJ, Simonian, Gregory V, Somers, Garrett, Spencer, M, Stevens, Daniel J, Tayar, Jamie, Treu, T, Valenti, Stefano, Van Saders, J, Villanueva, S, Villforth, C, Weiss, Yaniv, Winkler, H, and Zhu, W

Subjects
accretion, accretion disks, galaxies: individual, galaxies: Seyfert, astro-ph.GA, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry (incl. Structural), Astronomy & Astrophysics
Abstract

We present optical continuum lags for two Seyfert 1 galaxies, MCG+08-11-011 and NGC 2617, using monitoring data from a reverberation mapping campaign carried out in 2014. Our light curves span the ugriz filters over four months, with median cadences of 1.0 and 0.6 days for MCG+08-11-011 and NGC 2617, respectively, combined with roughly daily X-ray and near-UV data from Swift for NGC 2617. We find lags consistent with geometrically thin accretion-disk models that predict a lag-wavelength relation of τ ∝ λ 4/3. However, the observed lags are larger than predictions based on standard thin-disk theory by factors of 3.3 for MCG+08-11-011 and 2.3 for NGC 2617. These differences can be explained if the mass accretion rates are larger than inferred from the optical luminosity by a factor of 4.3 in MCG+08-11-011 and a factor of 1.3 in NGC 2617, although uncertainty in the SMBH masses determines the significance of this result. While the X-ray variability in NGC 2617 precedes the UV/optical variability, the long (2.6 day) lag is problematic for coronal reprocessing models.

Published
2018

10. Reverberation Mapping of Optical Emission Lines in Five Active Galaxies

Author

Fausnaugh, MM, Grier, CJ, Bentz, MC, Denney, KD, De Rosa, G, Peterson, BM, Kochanek, CS, Pogge, RW, Adams, SM, Barth, AJ, Beatty, Thomas G, Bhattacharjee, A, Borman, GA, Boroson, TA, Bottorff, MC, Brown, Jacob E, Brown, Jonathan S, Brotherton, MS, Coker, CT, Crawford, SM, Croxall, KV, Eftekharzadeh, Sarah, Eracleous, Michael, Joner, MD, Henderson, CB, Holoien, TW-S, Horne, Keith, Hutchison, T, Kaspi, Shai, Kim, S, King, Anthea L, Li, Miao, Lochhaas, Cassandra, Ma, Zhiyuan, MacInnis, F, Manne-Nicholas, ER, Mason, M, Montuori, Carmen, Mosquera, Ana, Mudd, Dale, Musso, R, Nazarov, SV, Nguyen, ML, Okhmat, DN, Onken, Christopher A, Ou-Yang, B, Pancoast, A, Pei, L, Penny, Matthew T, Poleski, Radosław, Rafter, Stephen, Romero-Colmenero, E, Runnoe, Jessie, Sand, David J, Schimoia, Jaderson S, Sergeev, SG, Shappee, BJ, Simonian, Gregory V, Somers, Garrett, Spencer, M, Starkey, DA, Stevens, Daniel J, Tayar, Jamie, Treu, T, Valenti, Stefano, Van Saders, J, Villanueva, S, Villforth, C, Weiss, Yaniv, Winkler, H, and Zhu, W

Subjects
galaxies: active, galaxies: individual, astro-ph.GA, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry (incl. Structural), Astronomy & Astrophysics
Abstract

We present the first results from an optical reverberation mapping campaign executed in 2014 targeting the active galactic nuclei (AGNs) MCG+08-11-011, NGC 2617, NGC 4051, 3C 382, and Mrk 374. Our targets have diverse and interesting observational properties, including a "changing look" AGN and a broad-line radio galaxy. Based on continuum-Hβ lags, we measure black hole masses for all five targets. We also obtain Hγ and He ii λ4686 lags for all objects except 3C 382. The He ii λ4686 lags indicate radial stratification of the BLR, and the masses derived from different emission lines are in general agreement. The relative responsivities of these lines are also in qualitative agreement with photoionization models. These spectra have extremely high signal-to-noise ratios (100-300 per pixel) and there are excellent prospects for obtaining velocity-resolved reverberation signatures.

Published
2017

11. Space Telescope and Optical Reverberation Mapping Project. V. Optical Spectroscopic Campaign and Emission-line Analysis for NGC 5548

Author

Pei, L, Fausnaugh, MM, Barth, AJ, Peterson, BM, Bentz, MC, De Rosa, G, Denney, KD, Goad, MR, Kochanek, CS, Korista, KT, Kriss, GA, Pogge, RW, Bennert, VN, Brotherton, M, Clubb, KI, Bontà, E Dalla, Filippenko, AV, Greene, JE, Grier, CJ, Vestergaard, M, Zheng, W, Adams, Scott M, Beatty, Thomas G, Bigley, A, Brown, Jacob E, Brown, Jonathan S, Canalizo, G, Comerford, JM, Coker, Carl T, Corsini, EM, Croft, S, Croxall, KV, Deason, AJ, Eracleous, Michael, Fox, OD, Gates, EL, Henderson, CB, Holmbeck, E, Holoien, TW-S, Jensen, JJ, Johnson, CA, Kelly, PL, Kim, S, King, A, Lau, MW, Li, Miao, Lochhaas, Cassandra, Ma, Zhiyuan, Manne-Nicholas, ER, Mauerhan, JC, Malkan, MA, McGurk, R, Morelli, L, Mosquera, Ana, Mudd, Dale, Sanchez, F Muller, Nguyen, ML, Ochner, P, Ou-Yang, B, Pancoast, A, Penny, Matthew T, Pizzella, A, Poleski, Radosław, Runnoe, Jessie, Scott, B, Schimoia, Jaderson S, Shappee, BJ, Shivvers, I, Simonian, Gregory V, Siviero, A, Somers, Garrett, Stevens, Daniel J, Strauss, MA, Tayar, Jamie, Tejos, N, Treu, T, Van Saders, J, Vican, L, Villanueva, S, Yuk, H, Zakamska, NL, Zhu, W, Anderson, MD, Arévalo, P, Bazhaw, C, Bisogni, S, Borman, GA, Bottorff, MC, Brandt, WN, Breeveld, AA, Cackett, EM, Carini, MT, Crenshaw, DM, De Lorenzo-Cáceres, A, Dietrich, M, Edelson, R, Efimova, NV, Ely, J, Evans, PA, and Ferland, GJ

Subjects
galaxies: active, galaxies: individual, galaxies: nuclei, galaxies: Seyfert, astro-ph.GA, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry (incl. Structural), Astronomy & Astrophysics
Abstract

We present the results of an optical spectroscopic monitoring program targeting NGC 5548 as part of a larger multiwavelength reverberation mapping campaign. The campaign spanned 6 months and achieved an almost daily cadence with observations from five ground-based telescopes. The Hβ and He ii λ4686 broad emission-line light curves lag that of the 5100 +-optical continuum by 4.17+0.36-0.36 and 0.79+0.35-0.34 days, respectively. The Hβ lag relative to the 1158 ultraviolet continuum light curve measured by the Hubble Space Telescope is ∼50% longer than that measured against the optical continuum, and the lag difference is consistent with the observed lag between the optical and ultraviolet continua. This suggests that the characteristic radius of the broad-line region is ∼50% larger than the value inferred from optical data alone. We also measured velocity-resolved emission-line lags for Hβ and found a complex velocity-lag structure with shorter lags in the line wings, indicative of a broad-line region dominated by Keplerian motion. The responses of both the Hβ and He ii emission lines to the driving continuum changed significantly halfway through the campaign, a phenomenon also observed for C iv, Lyα, He ii(+O iii]), and Si iv(+O iv]) during the same monitoring period. Finally, given the optical luminosity of NGC 5548 during our campaign, the measured Hβ lag is a factor of five shorter than the expected value implied by the R BLR-L AGN relation based on the past behavior of NGC 5548.

Published
2017

12. Revisiting the warm sub-Saturn TOI-1710b

Author

Orell-Miquel, J., Carleo, I., Murgas, F., Nowak, G., Pallé, E., Luque, R., Masseron, T., Sanz-Forcada, J., Dragomir, D., Dalba, P. A., Tronsgaard, R., Wittrock, J., Kim, K., Stibbards, C., Collins, K. I., Plavchan, P., Howell, S. B., Furlan, E., Buchhave, L. A., Gnilka, C. L., Gupta, A. F., Henning, Th, Lester, K. V., Rodriguez, J. E., Scott, N. J., Osborn, H. P., Villanueva, S., Seager, S., Winn, J. N., Jenkins, J. M., Vanderspek, R., Latham, D. W., Rowden, P., Watanabe, D., Torres, G., Burke, C. J., Daylan, T., Barclay, T., Twicken, J. D., Ricker, G. R., Orell-Miquel, J., Carleo, I., Murgas, F., Nowak, G., Pallé, E., Luque, R., Masseron, T., Sanz-Forcada, J., Dragomir, D., Dalba, P. A., Tronsgaard, R., Wittrock, J., Kim, K., Stibbards, C., Collins, K. I., Plavchan, P., Howell, S. B., Furlan, E., Buchhave, L. A., Gnilka, C. L., Gupta, A. F., Henning, Th, Lester, K. V., Rodriguez, J. E., Scott, N. J., Osborn, H. P., Villanueva, S., Seager, S., Winn, J. N., Jenkins, J. M., Vanderspek, R., Latham, D. W., Rowden, P., Watanabe, D., Torres, G., Burke, C. J., Daylan, T., Barclay, T., Twicken, J. D., and Ricker, G. R.

Published
2024

19. Robust Proportional-Derivative Control of a Three-Axis Milling Machine Tool

Author

Beltrán-Carbajal, F., Chavez-Conde, E., Villanueva, S., Damián, Z., Montes, E., Puerta, P., Pérez, R., Alvarez, G., Hutchison, David, editor, Kanade, Takeo, editor, Kittler, Josef, editor, Kleinberg, Jon M., editor, Mattern, Friedemann, editor, Mitchell, John C., editor, Naor, Moni, editor, Nierstrasz, Oscar, editor, Pandu Rangan, C., editor, Steffen, Bernhard, editor, Sudan, Madhu, editor, Terzopoulos, Demetri, editor, Tygar, Doug, editor, Vardi, Moshe Y., editor, Weikum, Gerhard, editor, Goebel, Randy, editor, Siekmann, Jörg, editor, Wahlster, Wolfgang, editor, Su, Chun-Yi, editor, Rakheja, Subhash, editor, and Liu, Honghai, editor

Published
2012
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20. Two long-period transiting exoplanets on eccentric orbits: NGTS-20 b (TOI-5152 b) and TOI-5153 b

Author

Ulmer-Moll, S., primary, Lendl, M., additional, Gill, S., additional, Villanueva, S., additional, Hobson, M. J., additional, Bouchy, F., additional, Brahm, R., additional, Dragomir, D., additional, Grieves, N., additional, Mordasini, C., additional, Anderson, D. R., additional, Acton, J. S., additional, Bayliss, D., additional, Bieryla, A., additional, Burleigh, M. R., additional, Casewell, S. L., additional, Chaverot, G., additional, Eigmüller, P., additional, Feliz, D., additional, Gaudi, B. S., additional, Gillen, E., additional, Goad, M. R., additional, Gupta, A. F., additional, Günther, M. N., additional, Henderson, B. A., additional, Henning, T., additional, Jenkins, J. S., additional, Jones, M., additional, Jordán, A., additional, Kendall, A., additional, Latham, D. W., additional, Mireles, I., additional, Moyano, M., additional, Nadol, J., additional, Osborn, H. P., additional, Pepper, J., additional, Pinto, M. T., additional, Psaridi, A., additional, Queloz, D., additional, Quinn, S., additional, Rojas, F., additional, Sarkis, P., additional, Schlecker, M., additional, Tilbrook, R. H., additional, Torres, P., additional, Trifonov, T., additional, Udry, S., additional, Vines, J. I., additional, West, R., additional, Wheatley, P., additional, Yao, X., additional, Zhao, Y., additional, and Zhou, G., additional

Published
2022
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27. How low can you go? SN 2018zd as a low-mass Fe core-collapse supernova

Author

Callis, E., Fraser, M., Pastorello, A., Dong, Subo, Brennan, S. J., Chen, P., Bose, S., Reynolds, T., Salmon, L., Jonker, P., Benetti, S., Berton, M., Cannizzaro, G., Cappellaro, E., Congiu, E., Dyrbye, S., Eappachen, D., Elias-Rosa, N., Gromadzki, M., Guti��rrez, C. P., Holmbo, S., Holoien, T. W. S., Itagaki, K., Kankare, E., Mattila, S., Mutel, R., Ochner, P., Post, R. S., Prieto, J., Reguitti, A., Roth, T., Ryon, J., Sagu��s-Carracedo, A., Shappee, B. J., Siviero, A., Stassun, K. G., Stritzinger, M., Tomasella, L., Villanueva, S., Wevers, T., and Wiggins, P.

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Astrophysics - Solar and Stellar Astrophysics, FOS: Physical sciences, Astrophysics - High Energy Astrophysical Phenomena, Solar and Stellar Astrophysics (astro-ph.SR)
Abstract

We present spectroscopy and photometry of SN 2018zd, a Type IIP core-collapse supernova with signatures of interaction with circumstantial material in its earliest spectra. High ionization lines, the earmark of shock breakout, are not seen in the earliest spectral epoch, and are only seen in a single spectrum at 4.9 d after explosion. The strength and brevity of these features imply a confined circumstellar material shell in the immediate vicinity of the progenitor. Once the narrow emission lines disappear, SN 2018zd evolves similarly to a Type IIP SN, although the blue colour and enhanced plateau magnitude of SN 2018zd suggests an additional source of luminosity throughout the plateau phase. While SN 2018zd has previously been proposed as an electron-capture SN, we suggest that it is an Fe core-collapse from a low mass red supergiant progenitor. Differences in interpretation for SN 2018zd arise in part due to the large uncertainty on the distance to the host-galaxy NGC 2146, which we re-derive here to be $15.6^{+6.1}_{-3.0}$ Mpc. We find the ejected $^{56}$Ni mass for SN 2018zd to be 0.017 M$_{\odot}$, significantly higher than models of ECSNe predict. We also find the Ni/Fe ratio in SN 2018zd to be much lower that would be expected for an ECSN.

Published
2021

33. Erratum: 'The Carnegie supernova project. I. Third photometry data release of low-redshift type Ia supernovae and other white dwarf explosions'

Author

Krisciunas, K., Contreras, C., Burns, C.R., Phillips, M.M., Hamuy, M., Stritzinger, M.D., Anais, J., Boldt, L., Busta, L., Campillay, A., Castellón, S., Folatelli, G., Freedman, W.L., González, C., Hsiao, E.Y., Krzeminski, W., Morrell, N., Persson, S.E., Roth, M, Salgado Cambiazo, F.J., Serón, J., Suntzeff, N.B., Torres, S., Filippenko, A.V., Li, W., Madore, B.F., Depoy, D.L., Marshall, J.L., Rheault, J.-P., and Villanueva, S.

Abstract

https://doi.org/10.3847/1538-3881/aa8df0This is an erratum for the article 2017 AJ 154 211

Published
2020

35. Neuroanatomy of the grey seal brain: Bringing pinnipeds into the neurobiological study of vocal learning

Author

Hoeksema, N., Verga, L., Mengede, J., Roessel, C. van, Villanueva, S., Salazar-Casals, A., Rubio-Garcia, A., Curcic-Blake, B., Vernes, S.C., Ravignani, A., Hoeksema, N., Verga, L., Mengede, J., Roessel, C. van, Villanueva, S., Salazar-Casals, A., Rubio-Garcia, A., Curcic-Blake, B., Vernes, S.C., and Ravignani, A.

Abstract

Contains fulltext : 237125.pdf (Author’s version preprint ) (Open Access), Comparative animal studies of complex behavioural traits, and their neurobiological underpinnings, can increase our understanding of their evolution, including in humans. Vocal learning, a potential precursor to human speech, is one such trait. Mammalian vocal learning is under-studied: most research has either focused on vocal learning in songbirds or its absence in non-human primates. Here, we focus on a highly promising model species for the neurobiology of vocal learning: grey seals (Halichoerus grypus). We provide a neuroanatomical atlas (based on dissected brain slices and magnetic resonance images), a labelled MRI template, a three-dimensional model with volumetric measurements of brain regions, and histological cortical stainings. Four main features of the grey seal brain stand out: (i) it is relatively big and highly convoluted; (ii) it hosts a relatively large temporal lobe and cerebellum; (iii) the cortex is similar to that of humans in thickness and shows the expected six-layered mammalian structure; (iv) there is expression of FoxP2 present in deeper layers of the cortex; FoxP2 is a gene involved in motor learning, vocal learning, and spoken language. Our results could facilitate future studies targeting the neural and genetic underpinnings of mammalian vocal learning, thus bridging the research gap from songbirds to humans and non-human primates. Our findings are relevant not only to vocal learning research but also to the study of mammalian neurobiology and cognition more in general.

Published
2021

36. Effect of the reduced graphene oxide (rGO) compaction degree and concentration on rGO-polymer composite printability and cell interactions

Author

Camara-Torres, M., Camara-Torres, M., Sinha, R., Eqtesadi, S., Wendelbo, R., Scatto, M., Scopece, P., Sanchez, A., Villanueva, S., Egizabal, A., Alvarez, N., Patelli, A., Mota, C., Moroni, L., Camara-Torres, M., Camara-Torres, M., Sinha, R., Eqtesadi, S., Wendelbo, R., Scatto, M., Scopece, P., Sanchez, A., Villanueva, S., Egizabal, A., Alvarez, N., Patelli, A., Mota, C., and Moroni, L.

Abstract

Graphene derivatives combined with polymers have attracted enormous attention for bone tissue engineering applications. Among others, reduced graphene oxide (rGO) is one of the preferred graphene-based fillers for the preparation of composites via melt compounding, and their further processing into 3D scaffolds, due to its established large-scale production method, thermal stability, and electrical conductivity. In this study, rGO (low bulk density 10 g L-1) was compacted by densification using a solvent (either acetone or water) prior to melt compounding, to simplify its handling and dosing into a twin-screw extrusion system. The effects of rGO bulk density (medium and high), densification solvent, and rGO concentration (3, 10 and 15% in weight) on rGO dispersion within the composite, electrical conductivity, printability and cell-material interactions were studied. High bulk density rGO (90 g L-1) occupied a low volume fraction within polymer composites, offering poor electrical properties but a reproducible printability up to 15 wt% rGO. On the other hand, the volume fraction within the composites of medium bulk density rGO (50 g L-1) was higher for a given concentration, enhancing rGO particle interactions and leading to enhanced electrical conductivity, but compromising the printability window. For a given bulk density (50 g L-1), rGO densified in water was more compacted and offered poorer dispersability within the polymer than rGO densified in acetone, and resulted in scaffolds with poor layer bonding or even lack of printability at high rGO percentages. A balance in printability and electrical properties was obtained for composites with medium bulk density achieved with rGO densified in acetone. Here, increasing rGO concentration led to more hydrophilic composites with a noticeable increase in protein adsorption. Moreover, scaffolds prepared with such composites presented antimicrobial properties even at low rGO contents (3 wt%). In addition, the viability a

Published
2021

37. ASASSN-18am/SN 2018gk:an overluminous Type IIb supernova from a massive progenitor

Author

Bose, Subhash, Dong, Subo, Kochanek, C. S., Stritzinger, M. D., Ashall, Chris, Benetti, Stefano, Falco, E., Filippenko, Alexei, Pastorello, Andrea, Prieto, Jose L., Somero, Auni, Sukhbold, Tuguldur, Zhang, Junbo, Auchettl, Katie, Brink, Thomas G., Brown, J. S., Chen, Ping, Fiore, A., Grupe, Dirk, Holoien, T. W. S., Lundqvist, Peter, Mattila, Seppo, Mutel, Robert, Pooley, David, Post, R. S., Reddy, Naveen, Reynolds, Thomas M., Shappee, Benjamin J., Stanek, K. Z., Thompson, Todd A., Villanueva, S. jR, Zheng, Weikang, Bose, Subhash, Dong, Subo, Kochanek, C. S., Stritzinger, M. D., Ashall, Chris, Benetti, Stefano, Falco, E., Filippenko, Alexei, Pastorello, Andrea, Prieto, Jose L., Somero, Auni, Sukhbold, Tuguldur, Zhang, Junbo, Auchettl, Katie, Brink, Thomas G., Brown, J. S., Chen, Ping, Fiore, A., Grupe, Dirk, Holoien, T. W. S., Lundqvist, Peter, Mattila, Seppo, Mutel, Robert, Pooley, David, Post, R. S., Reddy, Naveen, Reynolds, Thomas M., Shappee, Benjamin J., Stanek, K. Z., Thompson, Todd A., Villanueva, S. jR, and Zheng, Weikang

Abstract

ASASSN-18am/SN 2018gk is a newly discovered member of the rare group of luminous, hydrogen-rich supernovae (SNe) with a peak absolute magnitude of M-V approximate to -20 mag that is in between normal core-collapse SNe and superluminous SNe. These SNe show no prominent spectroscopic signatures of ejecta interacting with circumstellar material (CSM), and their powering mechanism is debated. ASASSN-18am declines extremely rapidly for a Type II SN, with a photospheric-phase decline rate of similar to 6.0 mag (100 d)(-1). Owing to the weakening of H I and the appearance of He I in its later phases, ASASSN-18am is spectroscopically a Type IIb SN with a partially stripped envelope. However, its photometric and spectroscopic evolution shows significant differences from typical SNe IIb. Using a radiative diffusion model, we find that the light curve requires a high synthesized Ni-56 mass M-Ni similar to 0.4 M-circle dot and ejecta with high kinetic energy E-kin = (7-10) x 10(51) erg. Introducing a magnetar central engine still requires M-Ni similar to 0.3 M-circle dot and E-kin = 3 x 10(51) erg. The high Ni-56 mass is consistent with strong iron-group nebular lines in its spectra, which are also similar to several SNe Ic-BL with high Ni-56 yields. The earliest spectrum shows 'flash ionization' features, from which we estimate a mass-loss rate of (M) over dot approximate to 2 x 10(-4 )M(circle dot) yr(-1). This wind density is too low to power the luminous light curve by ejecta-CSM interaction. We measure expansion velocities as high as 17 000 km s(-1) for H alpha, which is remarkably high compared to other SNe II. We estimate an oxygen core mass of 1.8-3.4 M-circle dot using the [O I] luminosity measured from a nebular-phase spectrum, implying a progenitor with a zero-age main-sequence mass of 19-26 M-circle dot.

Published
2021

38. Space Telescope and Optical Reverberation Mapping Project. IX. Velocity-Delay Maps for Broad Emission Lines in NGC 5548

Author

Horne, Keith, Rosa, G. De, Peterson, B. M., Barth, A. J., Ely, J., Fausnaugh, M. M., Kriss, G. A., Pei, L., Bentz, M. C., Cackett, E. M., Edelson, R., Eracleous, M., Goad, M. R., Grier, C. J., Kaastra, J., Kochanek, C. S., Krongold, Y., Mathur, S., Netzer, H., Proga, D., Tejos, N., Vestergaard, M., Villforth, C., Adams, S. M., Anderson, M. D., Arevalo, P., Beatty, T. G., Bennert, V. N., Bigley, A., Bisogni, S., Borman, G. A., Boroson, T. A., Bottorff, M. C., Brandt, W. N., Breeveld, A. A., Brotherton, M., Brown, J. E., Brown, J. S., Canalizo, G., Carini, M. T., Clubb, K. I., Comerford, J. M., Corsini, E. M., Crenshaw, D. M., Croft, S., Croxall, K. V., Bonta, E. Dalla, Deason, A. J., Dehghanian, M., Lorenzo-Caceres, A. De, Denney, K. D., Dietrich, M., Done, C., Efimova, N. V., Evans, P. A., Ferland, G. J., Filippenko, A. V., Flatland, K., Fox, O. D., Gardner, E., Gates, E. L., Gehrels, N., Geier, S., Gelbord, J. M., Gonzalez, L., Gorjian, V., Greene, J. E., Grupe, D., Gupta, A., Hall, P. B., Henderson, C. B., Hicks, S., Holmbeck, E., Holoien, T. W. -S., Hutchison, T., Im, M., Jensen, J. J., Johnson, C. A., Joner, M. D., Jones, J., Kaspi, S., Kelly, P. L., Kennea, J. A., Kim, M., Kim, S., Kim, S. C., King, A., Klimanov, S. A., Korista, K. T., Lau, M. W., Lee, J. C., Leonard, D. C., Li, Miao, Lira, P., Lochhaas, C., Ma, Zhiyuan, MacInnis, F., Malkan, M. A., Manne-Nicholas, E. R., Mauerhan, J. C., McGurk, R., McHardy, I. M., Montuori, C., Morelli, L., Mosquera, A., Mudd, D., Muller-Sanchez, F., Nazarov, S. V., Norris, R. P., Nousek, J. A., Nguyen, M. L., Ochner, P., Okhmat, D. N., Pancoast, A., Papadakis, I., Parks, J. R., Penny, M. T., Pizzella, A., Pogge, R. W., Poleski, R., Pott, J. -U., Rafter, S. E., Rix, H. -W., Runnoe, J., Saylor, D. A., Schimoia, J. S., Schnuelle, K., Scott, B., Sergeev, S. G., Shappee, B. J., Shivvers, I., Siegel, M., Simonian, G. V., Siviero, A., Skielboe, A., Somers, G., Spencer, M., Starkey, D., Stevens, D. J., Sung, H. -I., Tayar, J., Treu, T., Turner, C. S., Uttley, P., Van Saders, J., Vican, L., Villanueva, S., Weiss, Y., Woo, J. -H., Yan, H., Young, S., Yuk, H., Zheng, W., Zhu, W., Zu, Y., Horne, Keith, Rosa, G. De, Peterson, B. M., Barth, A. J., Ely, J., Fausnaugh, M. M., Kriss, G. A., Pei, L., Bentz, M. C., Cackett, E. M., Edelson, R., Eracleous, M., Goad, M. R., Grier, C. J., Kaastra, J., Kochanek, C. S., Krongold, Y., Mathur, S., Netzer, H., Proga, D., Tejos, N., Vestergaard, M., Villforth, C., Adams, S. M., Anderson, M. D., Arevalo, P., Beatty, T. G., Bennert, V. N., Bigley, A., Bisogni, S., Borman, G. A., Boroson, T. A., Bottorff, M. C., Brandt, W. N., Breeveld, A. A., Brotherton, M., Brown, J. E., Brown, J. S., Canalizo, G., Carini, M. T., Clubb, K. I., Comerford, J. M., Corsini, E. M., Crenshaw, D. M., Croft, S., Croxall, K. V., Bonta, E. Dalla, Deason, A. J., Dehghanian, M., Lorenzo-Caceres, A. De, Denney, K. D., Dietrich, M., Done, C., Efimova, N. V., Evans, P. A., Ferland, G. J., Filippenko, A. V., Flatland, K., Fox, O. D., Gardner, E., Gates, E. L., Gehrels, N., Geier, S., Gelbord, J. M., Gonzalez, L., Gorjian, V., Greene, J. E., Grupe, D., Gupta, A., Hall, P. B., Henderson, C. B., Hicks, S., Holmbeck, E., Holoien, T. W. -S., Hutchison, T., Im, M., Jensen, J. J., Johnson, C. A., Joner, M. D., Jones, J., Kaspi, S., Kelly, P. L., Kennea, J. A., Kim, M., Kim, S., Kim, S. C., King, A., Klimanov, S. A., Korista, K. T., Lau, M. W., Lee, J. C., Leonard, D. C., Li, Miao, Lira, P., Lochhaas, C., Ma, Zhiyuan, MacInnis, F., Malkan, M. A., Manne-Nicholas, E. R., Mauerhan, J. C., McGurk, R., McHardy, I. M., Montuori, C., Morelli, L., Mosquera, A., Mudd, D., Muller-Sanchez, F., Nazarov, S. V., Norris, R. P., Nousek, J. A., Nguyen, M. L., Ochner, P., Okhmat, D. N., Pancoast, A., Papadakis, I., Parks, J. R., Penny, M. T., Pizzella, A., Pogge, R. W., Poleski, R., Pott, J. -U., Rafter, S. E., Rix, H. -W., Runnoe, J., Saylor, D. A., Schimoia, J. S., Schnuelle, K., Scott, B., Sergeev, S. G., Shappee, B. J., Shivvers, I., Siegel, M., Simonian, G. V., Siviero, A., Skielboe, A., Somers, G., Spencer, M., Starkey, D., Stevens, D. J., Sung, H. -I., Tayar, J., Treu, T., Turner, C. S., Uttley, P., Van Saders, J., Vican, L., Villanueva, S., Weiss, Y., Woo, J. -H., Yan, H., Young, S., Yuk, H., Zheng, W., Zhu, W., and Zu, Y.

Abstract

In this contribution, we achieve the primary goal of the active galactic nucleus (AGN) STORM campaign by recovering velocity-delay maps for the prominent broad emission lines (Ly alpha, C IV, He II, and H beta) in the spectrum of NGC 5548. These are the most detailed velocity-delay maps ever obtained for an AGN, providing unprecedented information on the geometry, ionization structure, and kinematics of the broad-line region. Virial envelopes enclosing the emission-line responses show that the reverberating gas is bound to the black hole. A stratified ionization structure is evident. The He ii response inside 5-10 lt-day has a broad single-peaked velocity profile. The Ly alpha, C IV, and H beta responses extend from inside 2 to outside 20 lt-day, with double peaks at 2500 km s(-1) in the 10-20 lt-day delay range. An incomplete ellipse in the velocity-delay plane is evident in H beta. We interpret the maps in terms of a Keplerian disk with a well-defined outer rim at R = 20 lt-day. The far-side response is weaker than that from the near side. The line-center delay tau = (R/c)(1 - sin i) approximate to 5 days gives the inclination i approximate to 45 degrees. The inferred black hole mass is (BH) 7 x 10(7) M-circle dot. In addition to reverberations, the fit residuals confirm that emission-line fluxes are depressed during the "BLR Holiday" identified in previous work. Moreover, a helical "Barber-Pole" pattern, with stripes moving from red to blue across the C IV and Ly alpha line profiles, suggests azimuthal structure rotating with a 2 yr period that may represent precession or orbital motion of inner-disk structures casting shadows on the emission-line region farther out.

Published
2021

42. ASASSN-18am/SN 2018gk: an overluminous Type IIb supernova from a massive progenitor

Author

Bose, Subhash, primary, Dong, Subo, additional, Kochanek, C S, additional, Stritzinger, M D, additional, Ashall, Chris, additional, Benetti, Stefano, additional, Falco, E, additional, Filippenko, Alexei V, additional, Pastorello, Andrea, additional, Prieto, Jose L, additional, Somero, Auni, additional, Sukhbold, Tuguldur, additional, Zhang, Junbo, additional, Auchettl, Katie, additional, Brink, Thomas G, additional, Brown, J S, additional, Chen, Ping, additional, Fiore, A, additional, Grupe, Dirk, additional, Holoien, T W-S, additional, Lundqvist, Peter, additional, Mattila, Seppo, additional, Mutel, Robert, additional, Pooley, David, additional, Post, R S, additional, Reddy, Naveen, additional, Reynolds, Thomas M, additional, Shappee, Benjamin J, additional, Stanek, K Z, additional, Thompson, Todd A, additional, Villanueva, S, additional, and Zheng, WeiKang, additional

Published
2021
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43. 4CPS-268 Nivolumab versus pembrolizumab in secondline treatment of metastatic non-small cell lung cancer in clinical practice

Author

Valencia Soto, CM, primary, Villacañas Palomares, MV, additional, Martinez Callejo, V, additional, García-Avello Fernández-Cueto, A, additional, Barbadillo Villanueva, S, additional, Ochagavia Sufrategui, M, additional, Del Río Ortega, P, additional, Alonso Peralta, CA, additional, Garcia De La Paz, A, additional, and Valero Domínguez, M, additional

Published
2021
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46. Space Telescope and Optical Reverberation Mapping Project. IX. Velocity–Delay Maps for Broad Emission Lines in NGC 5548

Author

Horne, Keith, primary, Rosa, G. De, additional, Peterson, B. M., additional, Barth, A. J., additional, Ely, J., additional, Fausnaugh, M. M., additional, Kriss, G. A., additional, Pei, L., additional, Bentz, M. C., additional, Cackett, E. M., additional, Edelson, R., additional, Eracleous, M., additional, Goad, M. R., additional, Grier, C. J., additional, Kaastra, J., additional, Kochanek, C. S., additional, Krongold, Y., additional, Mathur, S., additional, Netzer, H., additional, Proga, D., additional, Tejos, N., additional, Vestergaard, M., additional, Villforth, C., additional, Adams, S. M., additional, Anderson, M. D., additional, Arévalo, P., additional, Beatty, T G., additional, Bennert, V. N., additional, Bigley, A., additional, Bisogni, S., additional, Borman, G. A., additional, Boroson, T. A., additional, Bottorff, M. C., additional, Brandt, W. N., additional, Breeveld, A. A., additional, Brotherton, M., additional, Brown, J. E., additional, Brown, J. S., additional, Canalizo, G., additional, Carini, M. T., additional, Clubb, K. I., additional, Comerford, J. M., additional, Corsini, E. M., additional, Crenshaw, D. M., additional, Croft, S., additional, Croxall, K. V., additional, Bontà, E. Dalla, additional, Deason, A. J., additional, Dehghanian, M., additional, Lorenzo-Cáceres, A. De, additional, Denney, K. D., additional, Dietrich, M., additional, Done, C., additional, Efimova, N. V., additional, Evans, P. A., additional, Ferland, G. J., additional, Filippenko, A. V., additional, Flatland, K., additional, Fox, O. D., additional, Gardner, E., additional, Gates, E. L., additional, Gehrels, N., additional, Geier, S., additional, Gelbord, J. M., additional, Gonzalez, L., additional, Gorjian, V., additional, Greene, J. E., additional, Grupe, D., additional, Gupta, A., additional, Hall, P. B., additional, Henderson, C. B., additional, Hicks, S., additional, Holmbeck, E., additional, Holoien, T. W.-S., additional, Hutchison, T., additional, Im, M., additional, Jensen, J. J., additional, Johnson, C. A., additional, Joner, M. D., additional, Jones, J., additional, Kaspi, S., additional, Kelly, P. L., additional, Kennea, J. A., additional, Kim, M., additional, Kim, S., additional, Kim, S. C., additional, King, A., additional, Klimanov, S. A., additional, Korista, K. T., additional, Lau, M. W., additional, Lee, J. C., additional, Leonard, D. C., additional, Li, Miao, additional, Lira, P., additional, Lochhaas, C., additional, Ma, Zhiyuan, additional, MacInnis, F., additional, Malkan, M. A., additional, Manne-Nicholas, E. R., additional, Mauerhan, J. C., additional, McGurk, R., additional, McHardy, I. M., additional, Montuori, C., additional, Morelli, L., additional, Mosquera, A., additional, Mudd, D., additional, Müller–Sánchez, F., additional, Nazarov, S. V., additional, Norris, R. P., additional, Nousek, J. A., additional, Nguyen, M. L., additional, Ochner, P., additional, Okhmat, D. N., additional, Pancoast, A., additional, Papadakis, I., additional, Parks, J. R., additional, Penny, M. T., additional, Pizzella, A., additional, Pogge, R. W., additional, Poleski, R., additional, Pott, J.-U., additional, Rafter, S. E., additional, Rix, H.-W., additional, Runnoe, J., additional, Saylor, D. A., additional, Schimoia, J. S., additional, Schnülle, K., additional, Scott, B., additional, Sergeev, S. G., additional, Shappee, B. J., additional, Shivvers, I., additional, Siegel, M., additional, Simonian, G. V., additional, Siviero, A., additional, Skielboe, A., additional, Somers, G., additional, Spencer, M., additional, Starkey, D., additional, Stevens, D. J., additional, Sung, H.-I., additional, Tayar, J., additional, Treu, T., additional, Turner, C. S., additional, Uttley, P., additional, Van Saders, J., additional, Vican, L., additional, Villanueva, S., additional, Weiss, Y., additional, Woo, J.-H., additional, Yan, H., additional, Young, S., additional, Yuk, H., additional, Zheng, W., additional, Zhu, W., additional, and Zu, Y., additional

Published
2021
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48. Space Telescope and Optical Reverberation Mapping Project. XII. Broad-line Region Modeling of NGC 5548

Author

Williams, P. R., primary, Pancoast, A., additional, Treu, T., additional, Brewer, B. J., additional, Peterson, B. M., additional, Barth, A. J., additional, Malkan, M. A., additional, Rosa, G. De, additional, Horne, Keith, additional, Kriss, G. A., additional, Arav, N., additional, Bentz, M. C., additional, Cackett, E. M., additional, Bontà, E. Dalla, additional, Dehghanian, M., additional, Done, C., additional, Ferland, G. J., additional, Grier, C. J., additional, Kaastra, J., additional, Kara, E., additional, Kochanek, C. S., additional, Mathur, S., additional, Mehdipour, M., additional, Pogge, R. W., additional, Proga, D., additional, Vestergaard, M., additional, Waters, T., additional, Adams, S. M., additional, Anderson, M. D., additional, Arévalo, P., additional, Beatty, T. G., additional, Bennert, V. N., additional, Bigley, A., additional, Bisogni, S., additional, Borman, G. A., additional, Boroson, T. A., additional, Bottorff, M. C., additional, Brandt, W. N., additional, Breeveld, A. A., additional, Brotherton, M., additional, Brown, J. E., additional, Brown, J. S., additional, Canalizo, G., additional, Carini, M. T., additional, Clubb, K. I., additional, Comerford, J. M., additional, Corsini, E. M., additional, Crenshaw, D. M., additional, Croft, S., additional, Croxall, K. V., additional, Deason, A. J., additional, Lorenzo-Cáceres, A. De, additional, Denney, K. D., additional, Dietrich, M., additional, Edelson, R., additional, Efimova, N. V., additional, Ely, J., additional, Evans, P. A., additional, Fausnaugh, M. M., additional, Filippenko, A. V., additional, Flatland, K., additional, Fox, O. D., additional, Gardner, E., additional, Gates, E. L., additional, Gehrels, N., additional, Geier, S., additional, Gelbord, J. M., additional, Gonzalez, L., additional, Gorjian, V., additional, Greene, J. E., additional, Grupe, D., additional, Gupta, A., additional, Hall, P. B., additional, Henderson, C. B., additional, Hicks, S., additional, Holmbeck, E., additional, Holoien, T. W.-S., additional, Hutchison, T., additional, Im, M., additional, Jensen, J. J., additional, Johnson, C. A., additional, Joner, M. D., additional, Jones, J., additional, Kaspi, S., additional, Kelly, P. L., additional, Kennea, J. A., additional, Kim, M., additional, Kim, S., additional, Kim, S. C., additional, King, A., additional, Klimanov, S. A., additional, Knigge, C., additional, Krongold, Y., additional, Lau, M. W., additional, Lee, J. C., additional, Leonard, D. C., additional, Li, Miao, additional, Lira, P., additional, Lochhaas, C., additional, Ma, Zhiyuan, additional, MacInnis, F., additional, Manne-Nicholas, E. R., additional, Mauerhan, J. C., additional, McGurk, R., additional, McHardy, I. M., additional, Montuori, C., additional, Morelli, L., additional, Mosquera, A., additional, Mudd, D., additional, Müller–Sánchez, F., additional, Nazarov, S. V., additional, Norris, R. P., additional, Nousek, J. A., additional, Nguyen, M. L., additional, Ochner, P., additional, Okhmat, D. N., additional, Papadakis, I., additional, Parks, J. R., additional, Pei, L., additional, Penny, M. T., additional, Pizzella, A., additional, Poleski, R., additional, Pott, J.-U., additional, Rafter, S. E., additional, Rix, H.-W., additional, Runnoe, J., additional, Saylor, D. A., additional, Schimoia, J. S., additional, Scott, B., additional, Sergeev, S. G., additional, Shappee, B. J., additional, Shivvers, I., additional, Siegel, M., additional, Simonian, G. V., additional, Siviero, A., additional, Skielboe, A., additional, Somers, G., additional, Spencer, M., additional, Starkey, D., additional, Stevens, D. J., additional, Sung, H.-I., additional, Tayar, J., additional, Tejos, N., additional, Turner, C. S., additional, Uttley, P., additional, Van Saders, J ., additional, Vaughan, S. A., additional, Vican, L., additional, Villanueva, S., additional, Villforth, C., additional, Weiss, Y., additional, Woo, J.-H., additional, Yan, H., additional, Young, S., additional, Yuk, H., additional, Zheng, W., additional, Zhu, W., additional, and Zu, Y., additional

Published
2020
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49. The TOI-763 system: sub-Neptunes orbiting a Sun-like star

Author

Fridlund, M, primary, Livingston, J, additional, Gandolfi, D, additional, Persson, C M, additional, Lam, K W F, additional, Stassun, K G, additional, Hellier, C, additional, Korth, J, additional, Hatzes, A P, additional, Malavolta, L, additional, Luque, R, additional, Redfield, S, additional, Guenther, E W, additional, Albrecht, S, additional, Barragan, O, additional, Benatti, S, additional, Bouma, L, additional, Cabrera, J, additional, Cochran, W D, additional, Csizmadia, S, additional, Dai, F, additional, Deeg, H J, additional, Esposito, M, additional, Georgieva, I, additional, Grziwa, S, additional, González Cuesta, L, additional, Hirano, T, additional, Jenkins, J M, additional, Kabath, P, additional, Knudstrup, E, additional, Latham, D W, additional, Mathur, S, additional, Mullally, S E, additional, Narita, N, additional, Nowak, G, additional, Olofsson, A O H, additional, Palle, E, additional, Pätzold, M, additional, Pompei, E, additional, Rauer, H, additional, Ricker, G, additional, Rodler, F, additional, Seager, S, additional, Serrano, L M, additional, Smith, A M S, additional, Spina, L, additional, Subjak, J, additional, Tenenbaum, P, additional, Ting, E B, additional, Vanderburg, A, additional, Vanderspek, R, additional, Van Eylen, V, additional, Villanueva, S, additional, and Winn, J N, additional

Published
2020
Full Text
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