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1. Visual-band brightnesses of Near Earth Objects that will be discovered in the infrared by NEO Surveyor

Author

Masiero, Joseph R., Linder, Tyler, Mainzer, Amy, Dahlen, Dar W., and Kwon, Yuna G.

Subjects
Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

NEO Surveyor will detect asteroids and comets using mid-infrared thermal emission, however ground-based followup resources will require knowledge of the expected visible light brightness in order to plan characterization observations. Here we describe the range of visual-to-infrared colors that the NEOs detected by Surveyor will span, and demonstrate that for objects that have no previously reported Visual band observations, estimates of the Johnson Visual-band brightness based on infrared flux alone will have significant uncertainty. Incidental or targeted photometric followup of objects discovered by Surveyor enables predictions of the fraction of reflected light visible and near-infrared wavelengths, supporting additional detailed characterization., Comment: 12 pages, 5 figures. Accepted for publication in PSJ

Published
2024

2. Optical Time-Series Photometry of the Symbiotic Nova V1835 Aquilae

Author

Caddy, Robert V., Layden, Andrew C., Reichart, Daniel E., Haislip, Joshua B., Kouprianov, Vladimir V., Ivarsen, Kevin M., Moore, Justin P., LaCluyze, Aaron P., Linder, Tyler R., and Nysewander, Melissa C.

Subjects
Astrophysics - Solar and Stellar Astrophysics
Abstract

We present time-series CCD photometry in the $BVRI$ passbands of the recently identified symbiotic nova V1835 Aquilae (NSV 11749) over an interval of 5.1 years with 7-14 day cadence, observed during its quiescence. We find slow light variations with a range of $\sim$0.9 mag in $V$ and $\sim$0.3 mag in $I$. Analysis of these data show strong periodicity at $419 \pm 10$ days, which we interpret to be the system's orbital period. A dip in the otherwise-sinusoidal phased light curve suggests a weak ellipsoidal effect due to tidal distortion of the giant star, which in turn opens the possibility that V1835 Aql transfers some of its mass to the hot component via Roche lobe overflow rather than via a stellar wind. We also find evidence that V1835 Aql is an S-type symbiotic star, relatively free of circumstellar dust, and include it among the nuclear burning group of symbiotics. Finally, we provide photometry, periods, and light curve classifications for 22 variable stars in the field around V1835 Aql, about half of which are newly identified., Comment: Main Paper: 28 pages, 5 figures, 5 tables. Supplement: 15 pages, 4 figures, 1 table. To be published in Publications of the Astronomical Society of the Pacific

Published
2022
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3. NEOWISE Observations Of The Potentially Hazardous Asteroid (99942) Apophis

Author

Satpathy, Akash, Mainzer, Amy, Masiero, Joseph R., Linder, Tyler, Cutri, Roc M., Wright, Edward L., Pittichova, Jana, Grav, Tommy, and Kramer, Emily

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

Large potentially hazardous asteroids (PHAs) are capable of causing a global catastrophe in the event of a planetary collision. Thus, rapid assessment of such an object's physical characteristics is crucial for determining its potential risk scale. We treated the near-Earth asteroid (99942) Apophis as a newly discovered object during its 2020-2021 close-approach as part of a mock planetary defense exercise. The object was detected by the Near-Earth Object Wide-field Infrared Survey Explorer (NEOWISE), and data collected by the two active bands (3.4 ${\mu}$m and 4.6 ${\mu}$m) were analyzed using thermal and thermophysical modeling. Our results indicate that Apophis is an elongated object with an effective spherical diameter D$_{eff}$ = 340 $\pm$ 70 m, a geometric visual albedo p$_{V}$ = 0.31 $\pm$ 0.09, and a thermal inertia $\Gamma$ $\sim$ 150 - 2850 Jm$^{-2}$s$^{-0.5}$K$^{-1}$ with a best-fit value of 550 Jm$^{-2}$s$^{-0.5}$K$^{-1}$. NEOWISE "discovery" observations reveal that (99942) Apophis is a potentially hazardous asteroid that would likely cause damage at a regional level and not a global one., Comment: 19 Pages, 6 Figures, Accepted for publication in PSJ

Published
2022

4. Space Weathering within C-Complex Main Belt Asteroid Families

Author

Thomas, Cristina A., Trilling, David E., Rivkin, Andrew S., and Linder, Tyler

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

Using data from the Sloan Digital Sky Survey Moving Object Catalog, we study color as a function of size for C-complex families in the Main Asteroid Belt to improve our understanding of space weathering of carbonaceous materials. We find two distinct spectral slope trends: Hygiea-type and Themis-type. The Hygiea-type families exhibit a reduction in spectral slope with increasing object size until a minimum slope value is reached and the trend reverses with increasing slope with increasing object size. The Themis family shows an increase in spectral slope with increasing object size until a maximum slope is reached and the spectral slope begins to decrease slightly or plateaus for the largest objects. Most families studied show the Hygiea-type trend. The processes responsible for these distinct changes in spectral slope affect several different taxonomic classes within the C-complex and appear to act quickly to alter the spectral slopes of the family members., Comment: 13 pages, 6 figures, 1 table, to be published in the Astronomical Journal

Published
2021
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5. Physical Characterization of Active Asteroid (6478) Gault

Author

Sanchez, Juan A., Reddy, Vishnu, Thirouin, Audrey, Wright, Edward L., Linder, Tyler R., Kareta, Theodore, and Sharkey, Benjamin

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

Main belt asteroid (6478) Gault has been dynamically linked with two overlapping asteroid families: Phocaea, dominated by S-type asteroids, and Tamara, dominated by low-albedo C-types. This object has recently become an interesting case for study, after images obtained in late 2018 revealed that it was active and displaying a comet-like tail. Previous authors have proposed that the most likely scenarios to explain the observed activity on Gault were rotational excitation or merger of near-contact binaries. Here we use new photometric and spectroscopic data of Gault to determine its physical and compositional properties. Lightcurves derived from the photometric data showed little variation over three nights of observations, which prevented us from determining the rotation period of the asteroid. Using WISE observations of Gault and the near-Earth Asteroid Thermal Model (NEATM) we determined that this asteroid has a diameter $<$6 km. NIR spectroscopic data obtained with the Infrared Telescope Facility (IRTF) showed a spectrum similar to that of S-complex asteroids, and a surface composition consistent with H chondrite meteorites. These results favor a compositional affinity between Gault and asteroid (25) Phocaea, and rules out a compositional link with the Tamara family. From the spectroscopic data we found no evidence of fresh material that could have been exposed during the outburst episodes., Comment: 9 pages, 4 figures, accepted for publication in ApJL

Published
2019
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6. New Pulse Timing Measurements of the sdBV Star CS 1246

Author

Hutchens, Zackary L., Barlow, Brad N., Soto, Alan Vasquez, Reichart, Dan E., Haislip, Josh B., Kouprianov, Vladimir V., Linder, Tyler R., and Moore, Justin P.

Subjects
Astrophysics - Solar and Stellar Astrophysics
Abstract

CS 1246 is a hot subdwarf B star discovered in 2009 to exhibit a single, large-amplitude radial pulsation. An O-C diagram constructed from this mode revealed reflex motion due to the presence of a low-mass M dwarf, as well as a long-term trend consistent with a decrease in the pulsational period. The orbital reflex motion was later confirmed with radial velocity measurements. Using eight years of data collected with the Skynet Robotic Telescope Network, we show that the pulsation amplitude of CS 1246 is decaying nonlinearly. We also present an updated O-C diagram, which might now indicate a positive $\dot P$ and a new $2.09 \pm 0.05$ yr oscillation consistent with orbital reflex motion of the entire inner sdB+dM binary, possibly due to the gravitational influence of a circumbinary planet with minimum mass $m\sin i = 3.3 \, \pm \, ^{2.1}_{1.2}$ $M_{\rm Jup}$. However, unlike the presence of the M dwarf, we hesitate to claim this object as a definitive detection since intrinsic variability of the pulsation phase could theoretically produce a similar effect., Comment: 6 pages, 4 figures, 2 tables; to appear in the Proceedings of the Eighth Meeting on Hot Subdwarfs and Related Objects, 9 to 15 July 2017, Cracow, Poland. Eds. A. Baran, A. E. Lynas-Gray, Open Astronomy, in press

Published
2017

7. A search for rapidly pulsating hot subdwarf stars in the GALEX survey

Author

Boudreaux, Emily M., Barlow, Brad N., Fleming, Scott W., Soto, Alan Vasquez, Million, Chase, Reichart, Dan E., Haislip, Josh B., Linder, Tyler R., and Moore, Justin P.

Subjects
Astrophysics - Solar and Stellar Astrophysics
Abstract

NASA's Galaxy Evolution Explorer (GALEX) provided near- and far-UV observations for approximately 77 percent of the sky over a ten-year period; however, the data reduction pipeline initially only released single NUV and FUV images to the community. The recently released Python module gPhoton changes this, allowing calibrated time-series aperture photometry to be extracted easily from the raw GALEX data set. Here we use gPhoton to generate light curves for all hot subdwarf B (sdB) stars that were observed by GALEX, with the intention of identifying short-period, p-mode pulsations. We find that the spacecraft's short visit durations, uneven gaps between visits, and dither pattern make the detection of hot subdwarf pulsations difficult. Nonetheless, we detect UV variations in four previously known pulsating targets and report their UV pulsation amplitudes and frequencies. Additionally, we find that several other sdB targets not previously known to vary show promising signals in their periodograms. Using optical follow-up photometry with the Skynet Robotic Telescope Network, we confirm p-mode pulsations in one of these targets, LAMOST J082517.99+113106.3, and report it as the most recent addition to the sdBVr class of variable stars., Comment: 11 Pages, 8 Figures, Accepted for publication in the Astrophysical Journal

Published
2017
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9. 2023 DZ2 Planetary Defense Campaign

Author

Universidad de Alicante. Departamento de Física, Ingeniería de Sistemas y Teoría de la Señal, Reddy, Vishnu, Kelley, Michael S., Benner, Lance, Dotson, Jessie, Erasmus, Nicolas, Farnocchia, Davide, Linder, Tyler, Masiero, Joseph R., Thomas, Cristina, Bauer, James M., Alarcon, Miguel R., Bacci, P., Bamberger, Daniel, Battle, Adam, Benkhaldoun, Zouhair, Betti, Guido, Birlan, Mirel, Brozovic, Marina, Burt, Brian, Cantillo, David C., Chandra, Sunil, Chomette, Gregoire, Coates, Ashley, DeMeo, Francesca, Devogèle, Maxime, Fatka, Petr, Ferrais, Marin, Fini, Paolo, van Gend, Carel, Giorgini, Jon D., Glamazda, Dmitry, Holmes, Robert, Hora, Joseph L., Horiuchi, Shinji, Hornoch, Kamil, Iozzi, Marco, Jacques, Cristóvão, Jehin, Emmanuel, Jiang, Hai, Kaiser, Galina, Kušnirák, Peter, Kuznetsov, Eduard, de León, Julia, Liakos, Alexios, Licandro, Javier, Lister, Tim, Liu, Jing, Lopez-Oquendo, Andy, Maestripieri, M., Mathias, Donovan, Micheli, Marco, Naidu, Shantanu P., Nastasi, Alessandro, Nedelcu, Alin, Petrescu, Elisabeta, Popescu, Marcel, Potter, Stephen B., Pravec, Petr, Sanchez, Juan, Santana-Ros, Toni, Serra-Ricart, M., Sioulas, Nick, Sonka, Adrian B., Squilloni, Alessio, Tombelli, Maura, Trelia, Madalina M., Trilling, David, Warner, Elizabeth M., Wells, Guy, Wheeler, Lorien, Wiles, Mike, Universidad de Alicante. Departamento de Física, Ingeniería de Sistemas y Teoría de la Señal, Reddy, Vishnu, Kelley, Michael S., Benner, Lance, Dotson, Jessie, Erasmus, Nicolas, Farnocchia, Davide, Linder, Tyler, Masiero, Joseph R., Thomas, Cristina, Bauer, James M., Alarcon, Miguel R., Bacci, P., Bamberger, Daniel, Battle, Adam, Benkhaldoun, Zouhair, Betti, Guido, Birlan, Mirel, Brozovic, Marina, Burt, Brian, Cantillo, David C., Chandra, Sunil, Chomette, Gregoire, Coates, Ashley, DeMeo, Francesca, Devogèle, Maxime, Fatka, Petr, Ferrais, Marin, Fini, Paolo, van Gend, Carel, Giorgini, Jon D., Glamazda, Dmitry, Holmes, Robert, Hora, Joseph L., Horiuchi, Shinji, Hornoch, Kamil, Iozzi, Marco, Jacques, Cristóvão, Jehin, Emmanuel, Jiang, Hai, Kaiser, Galina, Kušnirák, Peter, Kuznetsov, Eduard, de León, Julia, Liakos, Alexios, Licandro, Javier, Lister, Tim, Liu, Jing, Lopez-Oquendo, Andy, Maestripieri, M., Mathias, Donovan, Micheli, Marco, Naidu, Shantanu P., Nastasi, Alessandro, Nedelcu, Alin, Petrescu, Elisabeta, Popescu, Marcel, Potter, Stephen B., Pravec, Petr, Sanchez, Juan, Santana-Ros, Toni, Serra-Ricart, M., Sioulas, Nick, Sonka, Adrian B., Squilloni, Alessio, Tombelli, Maura, Trelia, Madalina M., Trilling, David, Warner, Elizabeth M., Wells, Guy, Wheeler, Lorien, and Wiles, Mike

Abstract

We present the results of a fourth planetary defense exercise, focused this time on the small near-Earth asteroid (NEA) 2023 DZ2 and conducted during its close approach to the Earth in 2023 March. The International Asteroid Warning Network (IAWN), with support from NASA's Planetary Defense Coordination Office (PDCO), has been coordinating planetary defense observational campaigns since 2017 to test the operational readiness of the global planetary defense capabilities. The last campaign focused on the NEA Apophis, and an outcome of that exercise was the need for a short burst campaign to replicate a real-life near-Earth object impact hazard scenario. The goal of the 2023 DZ2 campaign was to characterize the small NEA as a potential impactor and exercise the planetary defense system including observations, hypothetical risk assessment and risk prediction, and hazard communication with a short notice of just 24 hr. The entire campaign lasted about 10 days. The campaign team was divided into several working groups based on the characterization method: photometry, spectroscopy, thermal IR photometry and optical polarimetry, radar, and risk assessment. Science results from the campaign show that 2023 DZ2 has a rotation period of 6.2745 ± 0.0030 minutes; visible wavelength color photometry/spectroscopy/polarimetry and near-IR spectroscopy all point to an E-type taxonomic classification with surface composition analogous to aubrite meteorites; and radar observations show that the object has a diameter of 30 ± 10 m, consistent with the high albedo (0.49) derived from polarimetric and thermal IR observations.

Published
2024

10. New Pulse Timing Measurements of the sdBV Star CS 1246

Author

Hutchens Zackary L., Barlow Brad N., Soto Alan Vasquez, Reichart Dan E., Haislip Josh B., Kouprianov Vladimir V., Linder Tyler R., and Moore Justin P.

Subjects
stars, individual, cs 1246, oscillations, subdwarfs, techniques, miscellaneous, Astronomy, QB1-991
Abstract

CS 1246 is a hot subdwarf B star discovered in 2009 to exhibit a single, large-amplitude radial pulsation. An O-C diagram constructed from this mode revealed reflex motion due to the presence of a low-mass M dwarf, as well as a long-term trend consistent with a decrease in the pulsational period. The orbital reflex motion was later confirmed with radial velocity measurements. Using eight years of data collected with the Skynet Robotic Telescope Network, we show that the pulsation amplitude of CS 1246 is decaying nonlinearly. We also present an updated O-C diagram, which might now indicate a positive Ṗ and a new 2.09 ± 0.05 yr oscillation consistent with orbital reflex motion of the entire inner sdB+dM binary, possibly due to the gravitational influence of a circumbinary planet with minimum mass . However, unlike the presence of the M dwarf, we hesistate to claim this object as a definitive detection since intrinsic variability of the pulsation phase could theoretically produce a similar effect.

Published
2017
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11. The Second International Asteroid Warning Network Timing Campaign: 2005 LW3

Author

Farnocchia, Davide, Reddy, Vishnu, Bauer, James M., Warner, Elizabeth M., Micheli, Marco, Payne, Matthew J., Farnham, Tony, Kelley, Michael S., Alarcon, Miguel R., Bacci, Paolo, Bacci, Roberto, Bachini, Mauro, Baillie, Kevin, Baj, Giorgio, Bamberger, Daniel, Barkov, Anatoly P., Beck, Stefan, Betti, Guido, Biancalani, Enrico, Bolin, Bryce T., Briggs, David, Buzzi, Luca, Cheng, Haowen, Christensen, Eric, Coffano, Alessandro, Conversi, Luca, Demeautis, Christophe, Denneau, Larry, Desmars, Josselin, Djupvik, Anlaug A., Elenin, Leonid, Fini, Paolo, Felber, Tobias, Flynn, Randy, Galli, Gianni, Granvik, Mikael, Gray, Bill, Gray, Zuri, Grazzini, Luca, Hasubick, Werner, Hoffmann, Tobias, Holmes, Robert, Iozzi, Marco, Ivanov, Alexander L., Ivanov, Viktor A., Ivanova, Natalya V., Jacques, Cristóvão, Jiang, Hai, Zheng, Jinghui, Kasikov, Anni, Kim, Myung-Jin, Kumar, Balaji, Lee, Hee-Jae, Li, Bin, Liu, Jing, Licandro, Javier, Linder, Tyler, Lysenkov, Vadim E., Maestripieri, Martina, Mantero, Andrea, Marinello, Vladimiro, McCormick, Jennie, Moon, Darrel, Nastasi, Alessandro, Neill, James D., Neue, Guenther, Novichonok, Artem O., Ocaña, Francisco, Pizzetti, Gianpaolo, Pomazan, Anton, Purdum, Josiah N., Ratinaud, Christophe, Roh, Dong-Goo, Romanov, Filipp D., Ruocco, Nello, Santana-Ros, Toni, Scarmato, Toni, Schmalz, Anastasia, Schmalz, Sergei, Serra-Ricart, Miquel, Sherrod, Clay, Sioulas, Nick, Soffiantini, Andrea, Succi, Giacomo, Tholen, David J., Thomsen, Jeppe S., Thuillot, William, Wainscoat, Richard, Wells, Guy, Weryk, Robert, Yakovenko, Nikolai A., Yim, Hong-Suh, Zhai, Chengxing, Farnocchia, Davide, Reddy, Vishnu, Bauer, James M., Warner, Elizabeth M., Micheli, Marco, Payne, Matthew J., Farnham, Tony, Kelley, Michael S., Alarcon, Miguel R., Bacci, Paolo, Bacci, Roberto, Bachini, Mauro, Baillie, Kevin, Baj, Giorgio, Bamberger, Daniel, Barkov, Anatoly P., Beck, Stefan, Betti, Guido, Biancalani, Enrico, Bolin, Bryce T., Briggs, David, Buzzi, Luca, Cheng, Haowen, Christensen, Eric, Coffano, Alessandro, Conversi, Luca, Demeautis, Christophe, Denneau, Larry, Desmars, Josselin, Djupvik, Anlaug A., Elenin, Leonid, Fini, Paolo, Felber, Tobias, Flynn, Randy, Galli, Gianni, Granvik, Mikael, Gray, Bill, Gray, Zuri, Grazzini, Luca, Hasubick, Werner, Hoffmann, Tobias, Holmes, Robert, Iozzi, Marco, Ivanov, Alexander L., Ivanov, Viktor A., Ivanova, Natalya V., Jacques, Cristóvão, Jiang, Hai, Zheng, Jinghui, Kasikov, Anni, Kim, Myung-Jin, Kumar, Balaji, Lee, Hee-Jae, Li, Bin, Liu, Jing, Licandro, Javier, Linder, Tyler, Lysenkov, Vadim E., Maestripieri, Martina, Mantero, Andrea, Marinello, Vladimiro, McCormick, Jennie, Moon, Darrel, Nastasi, Alessandro, Neill, James D., Neue, Guenther, Novichonok, Artem O., Ocaña, Francisco, Pizzetti, Gianpaolo, Pomazan, Anton, Purdum, Josiah N., Ratinaud, Christophe, Roh, Dong-Goo, Romanov, Filipp D., Ruocco, Nello, Santana-Ros, Toni, Scarmato, Toni, Schmalz, Anastasia, Schmalz, Sergei, Serra-Ricart, Miquel, Sherrod, Clay, Sioulas, Nick, Soffiantini, Andrea, Succi, Giacomo, Tholen, David J., Thomsen, Jeppe S., Thuillot, William, Wainscoat, Richard, Wells, Guy, Weryk, Robert, Yakovenko, Nikolai A., Yim, Hong-Suh, and Zhai, Chengxing

Abstract

The Earth close approach of near-Earth asteroid 2005 LW3 on 2022 November 23 represented a good opportunity for a second observing campaign to test the timing accuracy of astrometric observation. With 82 participating stations, the International Asteroid Warning Network collected 1046 observations of 2005 LW3 around the time of the close approach. Compared to the previous timing campaign targeting 2019 XS, some individual observers were able to significantly improve the accuracy of their reported observation times. In particular, U.S. surveys achieved good timing performance. However, no broad, systematic improvement was achieved compared to the previous campaign, with an overall negative bias persisting among the different observers. The calibration of observing times and the mitigation of timing errors should be important future considerations for observers and orbit computers, respectively., Validerad;2023;Nivå 2;2023-12-12 (hanlid);For funding information see: https://doi.org/10.3847/PSJ/acfd22;Full text license: CC BY

Published
2023
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12. The Second International Asteroid Warning Network Timing Campaign: 2005 LW3

Author

Universidad de Alicante. Departamento de Física, Ingeniería de Sistemas y Teoría de la Señal, Universidad de Alicante. Instituto Universitario de Física Aplicada a las Ciencias y las Tecnologías, Farnocchia, Davide, Reddy, Vishnu, Bauer, James M., Warner, Elizabeth M., Micheli, Marco, Payne, Matthew J., Farnham, Tony, Kelley, Michael S., Alarcon, Miguel R., Bacci, P., Bacci, Roberto, Bachini, M., Baillié, Kevin, Baj, Giorgio, Bamberger, Daniel, Barkov, Anatoly P., Beck, Stefan, Betti, Guido, Biancalani, Enrico, Bolin, Bryce T., Briggs, David, Buzzi, Luca, Cheng, Haowen, Christensen, Eric, Coffano, Alessandro, Conversi, Luca, Demeautis, Christophe, Denneau, Larry, Desmars, Josselin, Djupvik, Anlaug A., Elenin, Leonid, Fini, Paolo, Felber, Tobias, Flynn, Randy, Galli, Gianni, Granvik, Mikael, Gray, Bill, Gray, Zuri, Grazzini, Luca, Hasubick, Werner, Hoffmann, Tobias, Holmes, Robert, Iozzi, Marco, Ivanov, Alexander L., Ivanov, Viktor A., Ivanova, Natalya V., Jacques, Cristóvão, Jiang, Hai, Jinghui, Zheng, Kasikov, Anni, Kim, Myung-Jin, Kumar, Balaji, Lee, Hee-Jae, Li, Bin, Liu, Jing, Licandro, Javier, Linder, Tyler, Lysenkov, Vadim E., Maestripieri, M., Mantero, Andrea, Marinello, Vladimiro, McCormick, Jennie, Moon, Darrel, Nastasi, Alessandro, Neill, James D., Neue, Guenther, Novichonok, Artem O., Ocaña, Francisco, Pizzetti, Gianpaolo, Pomazan, Anton, Purdum, Josiah N., Ratinaud, Christophe, Roh, Dong-Goo, Romanov, Filipp D., Ruocco, Nello, Santana-Ros, Toni, Scarmato, Toni, Schmalz, Anastasia, Schmalz, Sergei, Serra-Ricart, M., Sherrod, Clay, Sioulas, Nick, Soffiantini, Andrea, Succi, G., Tholen, David J., Thomsen, Jeppe S., Thuillot, William, Wainscoat, Richard, Wells, Guy, Weryk, Robert, Yakovenko, Nikolai A., Yim, Hong-Suh, Zhai, Chengxing, Universidad de Alicante. Departamento de Física, Ingeniería de Sistemas y Teoría de la Señal, Universidad de Alicante. Instituto Universitario de Física Aplicada a las Ciencias y las Tecnologías, Farnocchia, Davide, Reddy, Vishnu, Bauer, James M., Warner, Elizabeth M., Micheli, Marco, Payne, Matthew J., Farnham, Tony, Kelley, Michael S., Alarcon, Miguel R., Bacci, P., Bacci, Roberto, Bachini, M., Baillié, Kevin, Baj, Giorgio, Bamberger, Daniel, Barkov, Anatoly P., Beck, Stefan, Betti, Guido, Biancalani, Enrico, Bolin, Bryce T., Briggs, David, Buzzi, Luca, Cheng, Haowen, Christensen, Eric, Coffano, Alessandro, Conversi, Luca, Demeautis, Christophe, Denneau, Larry, Desmars, Josselin, Djupvik, Anlaug A., Elenin, Leonid, Fini, Paolo, Felber, Tobias, Flynn, Randy, Galli, Gianni, Granvik, Mikael, Gray, Bill, Gray, Zuri, Grazzini, Luca, Hasubick, Werner, Hoffmann, Tobias, Holmes, Robert, Iozzi, Marco, Ivanov, Alexander L., Ivanov, Viktor A., Ivanova, Natalya V., Jacques, Cristóvão, Jiang, Hai, Jinghui, Zheng, Kasikov, Anni, Kim, Myung-Jin, Kumar, Balaji, Lee, Hee-Jae, Li, Bin, Liu, Jing, Licandro, Javier, Linder, Tyler, Lysenkov, Vadim E., Maestripieri, M., Mantero, Andrea, Marinello, Vladimiro, McCormick, Jennie, Moon, Darrel, Nastasi, Alessandro, Neill, James D., Neue, Guenther, Novichonok, Artem O., Ocaña, Francisco, Pizzetti, Gianpaolo, Pomazan, Anton, Purdum, Josiah N., Ratinaud, Christophe, Roh, Dong-Goo, Romanov, Filipp D., Ruocco, Nello, Santana-Ros, Toni, Scarmato, Toni, Schmalz, Anastasia, Schmalz, Sergei, Serra-Ricart, M., Sherrod, Clay, Sioulas, Nick, Soffiantini, Andrea, Succi, G., Tholen, David J., Thomsen, Jeppe S., Thuillot, William, Wainscoat, Richard, Wells, Guy, Weryk, Robert, Yakovenko, Nikolai A., Yim, Hong-Suh, and Zhai, Chengxing

Abstract

The Earth close approach of near-Earth asteroid 2005 LW3 on 2022 November 23 represented a good opportunity for a second observing campaign to test the timing accuracy of astrometric observation. With 82 participating stations, the International Asteroid Warning Network collected 1046 observations of 2005 LW3 around the time of the close approach. Compared to the previous timing campaign targeting 2019 XS, some individual observers were able to significantly improve the accuracy of their reported observation times. In particular, U.S. surveys achieved good timing performance. However, no broad, systematic improvement was achieved compared to the previous campaign, with an overall negative bias persisting among the different observers. The calibration of observing times and the mitigation of timing errors should be important future considerations for observers and orbit computers, respectively.

Published
2023

13. Optical Time-series Photometry of the Symbiotic Nova V1835 Aquilae

Author

Caddy, Robert V., primary, Layden, Andrew C., additional, Reichart, Daniel E., additional, Haislip, Joshua B., additional, Kouprianov, Vladimir V., additional, Ivarsen, Kevin M., additional, Moore, Justin P., additional, LaCluyze, Aaron P., additional, Linder, Tyler R., additional, and Nysewander, Melissa C., additional

Published
2022
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18. A search for rapidly pulsating hot subdwarf stars in the GALEX survey

Author

Boudreaux, Thomas M., Barlow, Brad N., Fleming, Scott W., Soto, Alan Vasquez, Million, Chase, Reichart, Dan E., Haislip, Josh B., Linder, Tyler R., Moore, Justin P., Boudreaux, Thomas M., Barlow, Brad N., Fleming, Scott W., Soto, Alan Vasquez, Million, Chase, Reichart, Dan E., Haislip, Josh B., Linder, Tyler R., and Moore, Justin P.

Abstract

NASA's Galaxy Evolution Explorer (GALEX) provided near- and far-UV observations for approximately 77 percent of the sky over a ten-year period; however, the data reduction pipeline initially only released single NUV and FUV images to the community. The recently released Python module gPhoton changes this, allowing calibrated time-series aperture photometry to be extracted easily from the raw GALEX data set. Here we use gPhoton to generate light curves for all hot subdwarf B (sdB) stars that were observed by GALEX, with the intention of identifying short-period, p-mode pulsations. We find that the spacecraft's short visit durations, uneven gaps between visits, and dither pattern make the detection of hot subdwarf pulsations difficult. Nonetheless, we detect UV variations in four previously known pulsating targets and report their UV pulsation amplitudes and frequencies. Additionally, we find that several other sdB targets not previously known to vary show promising signals in their periodograms. Using optical follow-up photometry with the Skynet Robotic Telescope Network, we confirm p-mode pulsations in one of these targets, LAMOST J082517.99+113106.3, and report it as the most recent addition to the sdBVr class of variable stars., Comment: 11 Pages, 8 Figures, Accepted for publication in the Astrophysical Journal

Published
2017
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19. Rotational Study Of Ambiguous Taxonomic Type Asteroids

Author

Linder, Tyler

Subjects
2453, asteroids, IRTF, main-belt, SDSS, Wabash
Abstract

Researchers have been categorizing asteroids by color for decades in an attempt to better understand asteroid composition and potential links to the meteorite population. However, only recently through large data collection surveys like the Sloan Digital Sky Survey (SDSS) has the asteroid population as a whole been studied. This research will look at a subset of asteroids with the highest reflectivity differences as reported by Carvano et al. (2010) in order to answer the question: Can visible wavelength ambiguous taxonomic asteroid types be an indicator of a non-homogeneous surface? This research studied asteroid 2453 (Wabash) in great detailed with visible spectrophotometry and near-infrared spectra. The results show that although a minor non-homogeneous surface was identified the non-homogenous surface is the not the primary source of the SDSS detected taxonomic variation.

Published
2017

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