20,228 research outputs found
IgA nephropathy, the most common cause of glomerulonephritis, is linked to 6q22–23
19openopenAli G. Gharavi; Yan Yan; Francesco Scolari; F. Paolo Schena; Giovanni M. Frasca; Gian Marco Ghiggeri;
Kerry Cooper; Antonio Amoroso; Battista Fabio Viola; Graziana Battini10; Gianluca Caridi8; Cristina
Canova; Anita Farhi; Vairavan Subramanian; Carol Nelson-Williams; Sue Woodford; Bruce A. Julian;
Robert J. Wyatt; Richard P. LiftonAli G., Gharavi; Yan, Yan; Scolari, Francesco; F., Paolo Schena; Giovanni M., Frasca; Gian Marco, Ghiggeri; Kerry, Cooper; Antonio, Amoroso; Battista Fabio, Viola; Graziana, Battini10; Gianluca, Caridi8; Cristina, Canova; Anita, Farhi; Vairavan, Subramanian; Carol Nelson, Williams; Sue, Woodford; Bruce A., Julian; Robert J., Wyatt; Richard P., Lifto
REM near-IR and optical photometric monitoring of Pre-Main Sequence Stars in Orion
We performed an intensive photometric monitoring of the PMS stars falling in
a field of about 10x10 arc-minutes in the vicinity of the Orion Nebula Cluster
(ONC). Photometric data were collected between November 2006 and January 2007
with the REM telescope in the VRIJHK' bands. The largest number of observations
is in the I band (about 2700 images) and in J and H bands (about 500 images in
each filter). From the observed rotational modulation, induced by the presence
of surface inhomogeneities, we derived the rotation periods for 16 stars and
improved previous determinations for the other 13. The analysis of the spectral
energy distributions and, for some stars, of high-resolution spectra provided
us with the main stellar parameters (luminosity, effective temperature, mass,
age, and vsini). We also report the serendipitous detection of two strong
flares in two of these objects. In most cases, the light-curve amplitudes
decrease progressively from the R to H band as expected for cool starspots,
while in a few cases, they can only be modelled by the presence of hot spots,
presumably ascribable to magnetospheric accretion. The application of our own
spot model to the simultaneous light curves in different bands allowed us to
deduce the spot parameters and particularly to disentangle the spot temperature
and size effects on the observed light curves.Comment: 29 pages, 24 figure
All-sky search in early O3 LIGO data for continuous gravitational-wave signals from unknown neutron stars in binary systems
none1370sìRapidly spinning neutron stars are promising sources of continuous gravitational waves. Detecting such a signal would allow probing of the physical properties of matter under extreme conditions. A significant fraction of the known pulsar population belongs to binary systems. Searching for unknown neutron stars in binary systems requires specialized algorithms to address unknown orbital frequency modulations. We present a search for continuous gravitational waves emitted by neutron stars in binary systems in early data from the third observing run of the Advanced LIGO and Advanced Virgo detectors using the semicoherent, GPU-accelerated, binary sky hough pipeline. The search analyzes the most sensitive frequency band of the LIGO detectors, 50–300 Hz. Binary orbital parameters are split into four regions, comprising orbital periods of three to 45 days and projected semimajor axes of two to 40 light seconds. No detections are reported. We estimate the sensitivity of the search using simulated continuous wave signals, achieving the most sensitive results to date across the analyzed parameter space.openAbbott, R.; Abbott, T. D.; Abraham, S.; Acernese, F.; Ackley, K.; Adams, A.; Adams, C.; Adhikari, R. X.; Adya, V. B.; Affeldt, C.; Agarwal, D.; Agathos, M.; Agatsuma, K.; Aggarwal, N.; Aguiar, O. D.; Aiello, L.; Ain, A.; Ajith, P.; Aleman, K. M.; Allen, G.; Allocca, A.; Altin, P. A.; Amato, A.; Anand, S.; Ananyeva, A.; Anderson, S. B.; Anderson, W. G.; Angelova, S. V.; Ansoldi, S.; Antelis, J. M.; Antier, S.; Appert, S.; Arai, K.; Araya, M. C.; Areeda, J. S.; Arène, M.; Arnaud, N.; Aronson, S. M.; Arun, K. G.; Asali, Y.; Ashton, G.; Aston, S. M.; Astone, P.; Aubin, F.; Aufmuth, P.; AultONeal, K.; Austin, C.; Babak, S.; Badaracco, F.; Bader, M. K. M.; Bae, S.; Baer, A. M.; Bagnasco, S.; Bai, Y.; Baird, J.; Ball, M.; Ballardin, G.; Ballmer, S. W.; Bals, M.; Balsamo, A.; Baltus, G.; Banagiri, S.; Bankar, D.; Bankar, R. S.; Barayoga, J. C.; Barbieri, C.; Barish, B. C.; Barker, D.; Barneo, P.; Barnum, S.; Barone, F.; Barr, B.; Barsotti, L.; Barsuglia, M.; Barta, D.; Bartlett, J.; Barton, M. A.; Bartos, I.; Bassiri, R.; Basti, A.; Bawaj, M.; Bayley, J. C.; Baylor, A. C.; Bazzan, M.; Bécsy, B.; Bedakihale, V. M.; Bejger, M.; Belahcene, I.; Benedetto, V.; Beniwal, D.; Benjamin, M. G.; Bennett, T. F.; Bentley, J. D.; BenYaala, M.; Bergamin, F.; Berger, B. K.; Bernuzzi, S.; Bersanetti, D.; Bertolini, A.; Betzwieser, J.; Bhandare, R.; Bhandari, A. V.; Bhattacharjee, D.; Bhaumik, S.; Bidler, J.; Bilenko, I. A.; Billingsley, G.; Birney, R.; Birnholtz, O.; Biscans, S.; Bischi, M.; Biscoveanu, S.; Bisht, A.; Biswas, B.; Bitossi, M.; Bizouard, M.-A.; Blackburn, J. K.; Blackman, J.; Blair, C. D.; Blair, D. G.; Blair, R. M.; Bobba, F.; Bode, N.; Boer, M.; Bogaert, G.; Boldrini, M.; Bondu, F.; Bonilla, E.; Bonnand, R.; Booker, P.; Boom, B. A.; Bork, R.; Boschi, V.; Bose, N.; Bose, S.; Bossilkov, V.; Boudart, V.; Bouffanais, Y.; Bozzi, A.; Bradaschia, C.; Brady, P. R.; Bramley, A.; Branch, A.; Branchesi, M.; Brau, J. E.; Breschi, M.; Briant, T.; Briggs, J. H.; Brillet, A.; Brinkmann, M.; Brockill, P.; Brooks, A. F.; Brooks, J.; Brown, D. D.; Brunett, S.; Bruno, G.; Bruntz, R.; Bryant, J.; Buikema, A.; Bulik, T.; Bulten, H. J.; Buonanno, A.; Buscicchio, R.; Buskulic, D.; Byer, R. L.; Cadonati, L.; Caesar, M.; Cagnoli, G.; Cahillane, C.; Cain, H. W.; Bustillo, J. Calderón; Callaghan, J. D.; Callister, T. A.; Calloni, E.; Camp, J. B.; Canepa, M.; Cannavacciuolo, M.; Cannon, K. C.; Cao, H.; Cao, J.; Capote, E.; Carapella, G.; Carbognani, F.; Carlin, J. B.; Carney, M. F.; Carpinelli, M.; Carullo, G.; Carver, T. L.; Diaz, J. 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Hernandez; Heurs, M.; Hild, S.; Hill, P.; Hines, A. S.; Hochheim, S.; Hofman, D.; Hohmann, J. N.; Holgado, A. M.; Holland, N. A.; Hollows, I. J.; Holmes, Z. J.; Holt, K.; Holz, D. E.; Hopkins, P.; Hough, J.; Howell, E. J.; Hoy, C. G.; Hoyland, D.; Hreibi, A.; Hsu, Y.; Huang, Y.; Hübner, M. T.; Huddart, A. D.; Huerta, E. A.; Hughey, B.; Hui, V.; Husa, S.; Huttner, S. H.; Huxford, R.; Huynh-Dinh, T.; Idzkowski, B.; Iess, A.; Inchauspe, H.; Ingram, C.; Intini, G.; Isi, M.; Isleif, K.; Iyer, B. R.; JaberianHamedan, V.; Jacqmin, T.; Jadhav, S. J.; Jadhav, S. P.; James, A. L.; Jan, A. Z.; Jani, K.; Janssens, K.; Janthalur, N. N.; Jaranowski, P.; Jariwala, D.; Jaume, R.; Jenkins, A. C.; Jeunon, M.; Jia, W.; Jiang, J.; Johns, G. R.; Jones, A. W.; Jones, D. I.; Jones, J. D.; Jones, P.; Jones, R.; Jonker, R. J. G.; Ju, L.; Junker, J.; Kalaghatgi, C. V.; Kalogera, V.; Kamai, B.; Kandhasamy, S.; Kang, G.; Kanner, J. B.; Kao, Y.; Kapadia, S. J.; Kapasi, D. P.; Karathanasis, C.; Karki, S.; Kashyap, R.; Kasprzack, M.; Kastaun, W.; Katsanevas, S.; Katsavounidis, E.; Katzman, W.; Kaur, T.; Kawabe, K.; Kéfélian, F.; Keitel, D.; Key, J. S.; Khadka, S.; Khalili, F. Y.; Khan, I.; Khan, S.; Khazanov, E. A.; Khetan, N.; Khursheed, M.; Kijbunchoo, N.; Kim, C.; Kim, J. C.; Kim, K.; Kim, W. S.; Kim, Y.-M.; Kimball, C.; King, P. J.; Kinley-Hanlon, M.; Kirchhoff, R.; Kissel, J. S.; Kleybolte, L.; Klimenko, S.; Knee, A. M.; Knowles, T. D.; Knyazev, E.; Koch, P.; Koekoek, G.; Koley, S.; Kolitsidou, P.; Kolstein, M.; Komori, K.; Kondrashov, V.; Kontos, A.; Koper, N.; Korobko, M.; Kovalam, M.; Kozak, D. B.; Kringel, V.; Krishnendu, N. V.; Królak, A.; Kuehn, G.; Kuei, F.; Kumar, A.; Kumar, P.; Kumar, Rahul; Kumar, Rakesh; Kuns, K.; Kwang, S.; Laghi, D.; Lalande, E.; Lam, T. L.; Lamberts, A.; Landry, M.; Lane, B. B.; Lang, R. N.; Lange, J.; Lantz, B.; La Rosa, I.; Lartaux-Vollard, A.; Lasky, P. D.; Laxen, M.; Lazzarini, A.; Lazzaro, C.; Leaci, P.; Leavey, S.; Lecoeuche, Y. K.; Lee, H. M.; Lee, H. W.; Lee, J.; Lee, K.; Lehmann, J.; Lemaître, A.; Leon, E.; Leroy, N.; Letendre, N.; Levin, Y.; Leviton, J. N.; Li, A. K. Y.; Li, B.; Li, J.; Li, T. G. F.; Li, X.; Linde, F.; Linker, S. D.; Linley, J. N.; Littenberg, T. B.; Liu, J.; Liu, K.; Liu, X.; Llorens-Monteagudo, M.; Lo, R. K. L.; Lockwood, A.; Lollie, M. L.; London, L. T.; Longo, A.; Lopez, D.; Lorenzini, M.; Loriette, V.; Lormand, M.; Losurdo, G.; Lough, J. D.; Lousto, C. O.; Lovelace, G.; Lück, H.; Lumaca, D.; Lundgren, A. P.; Macas, R.; MacInnis, M.; Macleod, D. M.; MacMillan, I. A. O.; Macquet, A.; Hernandez, I. Magaña; Magaña-Sandoval, F.; Magazzù, C.; Magee, R. M.; Maggiore, R.; Majorana, E.; Maksimovic, I.; Maliakal, S.; Malik, A.; Man, N.; Mandic, V.; Mangano, V.; Mango, J. L.; Mansell, G. L.; Manske, M.; Mantovani, M.; Mapelli, M.; Marchesoni, F.; Marion, F.; Mark, Z.; Márka, S.; Márka, Z.; Markakis, C.; Markosyan, A. S.; Markowitz, A.; Maros, E.; Marquina, A.; Marsat, S.; Martelli, F.; Martin, I. W.; Martin, R. M.; Martinez, M.; Martinez, V.; Martinovic, K.; Martynov, D. V.; Marx, E. J.; Masalehdan, H.; Mason, K.; Massera, E.; Masserot, A.; Massinger, T. J.; Masso-Reid, M.; Mastrogiovanni, S.; Matas, A.; Mateu-Lucena, M.; Matichard, F.; Matiushechkina, M.; Mavalvala, N.; McCann, J. J.; McCarthy, R.; McClelland, D. E.; McClincy, P.; McCormick, S.; McCuller, L.; McGhee, G. I.; McGuire, S. C.; McIsaac, C.; McIver, J.; McManus, D. J.; McRae, T.; McWilliams, S. T.; Meacher, D.; Mehmet, M.; Mehta, A. K.; Melatos, A.; Melchor, D. A.; Mendell, G.; Menendez-Vazquez, A.; Menoni, C. S.; Mercer, R. A.; 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Six months of mass outflow and inclined rings in the ejecta of V1494 Aql
V1494 Aql was a very fast nova which reached a visual maximum of mv≃ 4.0 by the end of 1999 December 3. We report observations from 4 to 284 d after discovery, including submillimetre- and centimetre-band fluxes, a single MERLIN image and optical spectroscopy in the 410 to 700 nm range. The extent of the radio continuum emission is consistent with a recent lower distance estimate of 1.6 kpc. We conclude that the optical and radio emission arises from the same expanding ejecta. We show that these observations are not consistent with simple kinematical spherical shell models used in the past to explain the rise and fall of the radio flux density in these objects. The resolved remnant structure is consistent with an inclined ring of enhanced density within the ejecta. Optical spectroscopy indicates likely continued mass ejection for over 195 d, with the material becoming optically thin in the visible sometime between 195 and 285 d after outburst
Contemporaneous broad-band photometry and H observations of T Tauri stars
The study of contemporaneous variations of the continuum flux and emission
lines is of great importance to understand the different astrophysical
processes at work in T Tauri stars. In this paper we present the results of a
simultaneous and H photometric monitoring, contemporaneous to
medium-resolution spectroscopy of six T Tauri stars in the Taurus-Auriga star
forming region. We have characterized the H photometric system using
synthetic templates and the contemporaneous spectra of the targets. We show
that we can achieve a precision corresponding to 23 \AA\ in the H
equivalent width, in typical observing conditions. The spectral analysis has
allowed us to determine the basic stellar parameters and the values of
quantities related to the accretion. In particular, we have measured a
significant veiling only for the three targets with the strongest H
emission (T Tau, FM Tau, and DG Tau). The broad-band photometric variations are
found to be in the range 0.050.70 mag and are often paired to variations in
the H intensity, which becomes stronger when the stellar continuum is
weaker. In addition, we have mostly observed a redder and a bluer
color as the stars become fainter. For most of the targets, the timescales of
these variations seem to be longer than the rotation period. One exception is T
Tau, for which the broad-band photometry varies with the rotation period. The
most plausible interpretation of these photometric and H variations is
that they are due to non-stationary mass accretion onto the stars, but
rotational modulation can play a major role in some cases.Comment: 21 pages, 11 figures, accepted for publication in Acta Astronomic
Student Comments
Comments on court cases by Jon R. Robinson, Leslie L. Clune, Joanne M. Frasca, Timothy J. McDevitt, Thomas Stalzer, Susan Finneran, William J. Brooks, III, Richard James Annen, Patricia S. Higgins, Jane M. Grote, Martin J. Hagan, Roger P. Balog, Bruce Meagher, Joseph L. Baldino, John E. Glennon, John Gaal, Joseph V. Rizzi, and Michael T. Bierman
On the nature of V2282 Sgr
The star V2282 Sgr is positionally consistent with a strong Chandra X-ray and
a Spitzer/IRAC MIR source. We derived its long term -band light curve from
the photographic archives of the Asiago and Catania Observatories, covering the
years from 1965 to 1984. CCD photometry in Summer 2009 was re-analyzed.
Optical spectra were secured at Loiano Observatory in 2011 and 2012. J H K
photometry, obtained from several experiments in different epochs was compared
and the Spitzer images were re-analyzed.
V2282 Sgr was found to be irregular variable in all wavelengths.
Spectroscopically, it shows strong emission features (H Balmer lines, [NII]6584
AA and [OIII]5007/4959 AA) while the Na D doublet is very strong, indicating a
circumstellar envelope. A single thermal energy distribution cannot reproduce
the observed SED, while it can be explained as the sum of a G-type star plus a
variable circumstellar disc, which mimics a class 0/I object. Most likely,
V2282 Sgr is a 1-2 mass pre main sequence star with an accretion
disk.Comment: 13 pages, 7 figure, in press on Baltic Astronom
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