adsabs/AstroCLIMB huggingface dataset:
Paper: GRANDMA and HXMT Observations of GRB 221009A: The Standard Luminosity Afterglow of a Hyperluminous Gamma-Ray Burst—In Gedenken an David Alexander Kann
Authors: D. A. Kann, S. Agayeva, V. Aivazyan, S. Alishov, C. M. Andrade, S. Antier, A. Baransky, P. Bendjoya, Z. Benkhaldoun, S. Beradze, D. Berezin, M. Boër, E. Broens, S. Brunier, M. Bulla, O. Burkhonov, E. Burns, Y. Chen, Y. P. Chen, M. Conti, M. W. Coughlin, W. W. Cui, F. Daigne, B. Delaveau, H. A. R. Devillepoix, T. Dietrich, D. Dornic, F. Dubois, J.-G. Ducoin, E. Durand, P.-A. Duverne, H.-B. Eggenstein, S. Ehgamberdiev, A. Fouad, M. Freeberg, D. Froebrich, M. Y. Ge, S. Gervasoni, V. Godunova, P. Gokuldass, E. Gurbanov, D. W. Han, E. Hasanov, P. Hello, T. Hussenot-Desenonges, R. Inasaridze, A. Iskandar, N. Ismailov, A. Janati, T. Jegou du Laz, S. M. Jia, S. Karpov, A. Kaeouach, R. W. Kiendrebeogo, A. Klotz, R. Kneip, N. Kochiashvili, N. Kunert, A. Lekic, S. Leonini, C. K. Li, W. Li, X. B. Li, J. Y. Liao, L. Logie, F. J. Lu, J. Mao, D. Marchais, R. Ménard, D. Morris, R. Natsvlishvili, V. Nedora, K. Noonan, K. Noysena, N. B. Orange, P. T. H. Pang, H. W. Peng, C. Pellouin, J. Peloton, T. Pradier, O. Pyshna, Y. Rajabov, S. Rau, C. Rinner, J.-P. Rivet, F. D. Romanov, P. Rosi, V. A. Rupchandani, M. Serrau, A. Shokry, A. Simon, K. Smith, O. Sokoliuk, M. Soliman, L. M. Song, A. Takey, Y. Tillayev, L. M. Tinjaca Ramirez, I. Tosta e Melo, D. Turpin, A. de Ugarte Postigo, S. Vanaverbeke, V. Vasylenko, D. Vernet, Z. Vidadi, C. Wang, J. Wang, L. T. Wang, X. F. Wang, S. L. Xiong, Y. P. Xu, W. C. Xue, X. Zeng, S. N. Zhang, H. S. Zhao, X. F. Zhao
Figure caption: The NMMA posterior distribution (shown are 90% confidence intervals) for our selected data sets when using different jet models of afterglowpy analyzing the GRANDMA data.
Paper: GRANDMA and HXMT Observations of GRB 221009A: The Standard Luminosity Afterglow of a Hyperluminous Gamma-Ray Burst—In Gedenken an David Alexander Kann
Authors: D. A. Kann, S. Agayeva, V. Aivazyan, S. Alishov, C. M. Andrade, S. Antier, A. Baransky, P. Bendjoya, Z. Benkhaldoun, S. Beradze, D. Berezin, M. Boër, E. Broens, S. Brunier, M. Bulla, O. Burkhonov, E. Burns, Y. Chen, Y. P. Chen, M. Conti, M. W. Coughlin, W. W. Cui, F. Daigne, B. Delaveau, H. A. R. Devillepoix, T. Dietrich, D. Dornic, F. Dubois, J.-G. Ducoin, E. Durand, P.-A. Duverne, H.-B. Eggenstein, S. Ehgamberdiev, A. Fouad, M. Freeberg, D. Froebrich, M. Y. Ge, S. Gervasoni, V. Godunova, P. Gokuldass, E. Gurbanov, D. W. Han, E. Hasanov, P. Hello, T. Hussenot-Desenonges, R. Inasaridze, A. Iskandar, N. Ismailov, A. Janati, T. Jegou du Laz, S. M. Jia, S. Karpov, A. Kaeouach, R. W. Kiendrebeogo, A. Klotz, R. Kneip, N. Kochiashvili, N. Kunert, A. Lekic, S. Leonini, C. K. Li, W. Li, X. B. Li, J. Y. Liao, L. Logie, F. J. Lu, J. Mao, D. Marchais, R. Ménard, D. Morris, R. Natsvlishvili, V. Nedora, K. Noonan, K. Noysena, N. B. Orange, P. T. H. Pang, H. W. Peng, C. Pellouin, J. Peloton, T. Pradier, O. Pyshna, Y. Rajabov, S. Rau, C. Rinner, J.-P. Rivet, F. D. Romanov, P. Rosi, V. A. Rupchandani, M. Serrau, A. Shokry, A. Simon, K. Smith, O. Sokoliuk, M. Soliman, L. M. Song, A. Takey, Y. Tillayev, L. M. Tinjaca Ramirez, I. Tosta e Melo, D. Turpin, A. de Ugarte Postigo, S. Vanaverbeke, V. Vasylenko, D. Vernet, Z. Vidadi, C. Wang, J. Wang, L. T. Wang, X. F. Wang, S. L. Xiong, Y. P. Xu, W. C. Xue, X. Zeng, S. N. Zhang, H. S. Zhao, X. F. Zhao
Figure caption: The UVOIR light curve of GRB 221009A (see Section 3.1). The magnitudes, expressed in the Vega system, are corrected for the SF11 galactic extinction. The break slope is at ∼0.6 day post-GRB trigger time between α 1 and α 2.
Paper: GRANDMA and HXMT Observations of GRB 221009A: The Standard Luminosity Afterglow of a Hyperluminous Gamma-Ray Burst—In Gedenken an David Alexander Kann
Authors: D. A. Kann, S. Agayeva, V. Aivazyan, S. Alishov, C. M. Andrade, S. Antier, A. Baransky, P. Bendjoya, Z. Benkhaldoun, S. Beradze, D. Berezin, M. Boër, E. Broens, S. Brunier, M. Bulla, O. Burkhonov, E. Burns, Y. Chen, Y. P. Chen, M. Conti, M. W. Coughlin, W. W. Cui, F. Daigne, B. Delaveau, H. A. R. Devillepoix, T. Dietrich, D. Dornic, F. Dubois, J.-G. Ducoin, E. Durand, P.-A. Duverne, H.-B. Eggenstein, S. Ehgamberdiev, A. Fouad, M. Freeberg, D. Froebrich, M. Y. Ge, S. Gervasoni, V. Godunova, P. Gokuldass, E. Gurbanov, D. W. Han, E. Hasanov, P. Hello, T. Hussenot-Desenonges, R. Inasaridze, A. Iskandar, N. Ismailov, A. Janati, T. Jegou du Laz, S. M. Jia, S. Karpov, A. Kaeouach, R. W. Kiendrebeogo, A. Klotz, R. Kneip, N. Kochiashvili, N. Kunert, A. Lekic, S. Leonini, C. K. Li, W. Li, X. B. Li, J. Y. Liao, L. Logie, F. J. Lu, J. Mao, D. Marchais, R. Ménard, D. Morris, R. Natsvlishvili, V. Nedora, K. Noonan, K. Noysena, N. B. Orange, P. T. H. Pang, H. W. Peng, C. Pellouin, J. Peloton, T. Pradier, O. Pyshna, Y. Rajabov, S. Rau, C. Rinner, J.-P. Rivet, F. D. Romanov, P. Rosi, V. A. Rupchandani, M. Serrau, A. Shokry, A. Simon, K. Smith, O. Sokoliuk, M. Soliman, L. M. Song, A. Takey, Y. Tillayev, L. M. Tinjaca Ramirez, I. Tosta e Melo, D. Turpin, A. de Ugarte Postigo, S. Vanaverbeke, V. Vasylenko, D. Vernet, Z. Vidadi, C. Wang, J. Wang, L. T. Wang, X. F. Wang, S. L. Xiong, Y. P. Xu, W. C. Xue, X. Zeng, S. N. Zhang, H. S. Zhao, X. F. Zhao
Figure caption: Same as Figure 5, but now all afterglows are in the z = 1 system. This means that the afterglow magnitudes have been additionally corrected for host-galaxy extinction, and all of them have been shifted to z = 1, taking the individual spectral slopes β and cosmological k-correction into account. We again highlight the afterglows of the bright nearby GRBs 030329 and 130427 and three solutions for GRB 221009A: the pure MW solution, SF11 MW extinction, and RF09 MW extinction, along with the respective host-galaxy solutions. All yield similar brightness, with the SF11 and RF09 results essentially overlapping (offset by only 0.05 mag), and the afterglow is seen to be among the more luminous ones detected so far. We note that the late afterglow of GRB 221009A is not corrected for a potential SN contribution; therefore, the luminosity may be overestimated.
Paper: GRANDMA and HXMT Observations of GRB 221009A: The Standard Luminosity Afterglow of a Hyperluminous Gamma-Ray Burst—In Gedenken an David Alexander Kann
Authors: D. A. Kann, S. Agayeva, V. Aivazyan, S. Alishov, C. M. Andrade, S. Antier, A. Baransky, P. Bendjoya, Z. Benkhaldoun, S. Beradze, D. Berezin, M. Boër, E. Broens, S. Brunier, M. Bulla, O. Burkhonov, E. Burns, Y. Chen, Y. P. Chen, M. Conti, M. W. Coughlin, W. W. Cui, F. Daigne, B. Delaveau, H. A. R. Devillepoix, T. Dietrich, D. Dornic, F. Dubois, J.-G. Ducoin, E. Durand, P.-A. Duverne, H.-B. Eggenstein, S. Ehgamberdiev, A. Fouad, M. Freeberg, D. Froebrich, M. Y. Ge, S. Gervasoni, V. Godunova, P. Gokuldass, E. Gurbanov, D. W. Han, E. Hasanov, P. Hello, T. Hussenot-Desenonges, R. Inasaridze, A. Iskandar, N. Ismailov, A. Janati, T. Jegou du Laz, S. M. Jia, S. Karpov, A. Kaeouach, R. W. Kiendrebeogo, A. Klotz, R. Kneip, N. Kochiashvili, N. Kunert, A. Lekic, S. Leonini, C. K. Li, W. Li, X. B. Li, J. Y. Liao, L. Logie, F. J. Lu, J. Mao, D. Marchais, R. Ménard, D. Morris, R. Natsvlishvili, V. Nedora, K. Noonan, K. Noysena, N. B. Orange, P. T. H. Pang, H. W. Peng, C. Pellouin, J. Peloton, T. Pradier, O. Pyshna, Y. Rajabov, S. Rau, C. Rinner, J.-P. Rivet, F. D. Romanov, P. Rosi, V. A. Rupchandani, M. Serrau, A. Shokry, A. Simon, K. Smith, O. Sokoliuk, M. Soliman, L. M. Song, A. Takey, Y. Tillayev, L. M. Tinjaca Ramirez, I. Tosta e Melo, D. Turpin, A. de Ugarte Postigo, S. Vanaverbeke, V. Vasylenko, D. Vernet, Z. Vidadi, C. Wang, J. Wang, L. T. Wang, X. F. Wang, S. L. Xiong, Y. P. Xu, W. C. Xue, X. Zeng, S. N. Zhang, H. S. Zhao, X. F. Zhao
Figure caption: Afterglow light curve of GRB 221009A in the context of a large sample of GRB afterglows (Kann et al. 2006, 2010, 2011, 2023a, 2023b, in preparation). These data have been corrected for Galactic extinction along each individual line of sight and, if possible, for the host-galaxy and SN contribution. For the GRB 221009A afterglow, we show the result for SF11 Galactic extinction. We highlight the afterglows of two other GRBs, namely, that of the much less energetic but similarly distant GRB 030329 and that of the well-studied, ultrabright GRB 130427A, which had been the closest highly energetic (“cosmological”) GRB so far. Assuming the higher extinction correction, the afterglow of GRB 221009A is seen to be the brightest that has ever been detected, even brighter than the afterglow of GRB 030329—however, by only a small margin.
Paper: GRANDMA and HXMT Observations of GRB 221009A: The Standard Luminosity Afterglow of a Hyperluminous Gamma-Ray Burst—In Gedenken an David Alexander Kann
Authors: D. A. Kann, S. Agayeva, V. Aivazyan, S. Alishov, C. M. Andrade, S. Antier, A. Baransky, P. Bendjoya, Z. Benkhaldoun, S. Beradze, D. Berezin, M. Boër, E. Broens, S. Brunier, M. Bulla, O. Burkhonov, E. Burns, Y. Chen, Y. P. Chen, M. Conti, M. W. Coughlin, W. W. Cui, F. Daigne, B. Delaveau, H. A. R. Devillepoix, T. Dietrich, D. Dornic, F. Dubois, J.-G. Ducoin, E. Durand, P.-A. Duverne, H.-B. Eggenstein, S. Ehgamberdiev, A. Fouad, M. Freeberg, D. Froebrich, M. Y. Ge, S. Gervasoni, V. Godunova, P. Gokuldass, E. Gurbanov, D. W. Han, E. Hasanov, P. Hello, T. Hussenot-Desenonges, R. Inasaridze, A. Iskandar, N. Ismailov, A. Janati, T. Jegou du Laz, S. M. Jia, S. Karpov, A. Kaeouach, R. W. Kiendrebeogo, A. Klotz, R. Kneip, N. Kochiashvili, N. Kunert, A. Lekic, S. Leonini, C. K. Li, W. Li, X. B. Li, J. Y. Liao, L. Logie, F. J. Lu, J. Mao, D. Marchais, R. Ménard, D. Morris, R. Natsvlishvili, V. Nedora, K. Noonan, K. Noysena, N. B. Orange, P. T. H. Pang, H. W. Peng, C. Pellouin, J. Peloton, T. Pradier, O. Pyshna, Y. Rajabov, S. Rau, C. Rinner, J.-P. Rivet, F. D. Romanov, P. Rosi, V. A. Rupchandani, M. Serrau, A. Shokry, A. Simon, K. Smith, O. Sokoliuk, M. Soliman, L. M. Song, A. Takey, Y. Tillayev, L. M. Tinjaca Ramirez, I. Tosta e Melo, D. Turpin, A. de Ugarte Postigo, S. Vanaverbeke, V. Vasylenko, D. Vernet, Z. Vidadi, C. Wang, J. Wang, L. T. Wang, X. F. Wang, S. L. Xiong, Y. P. Xu, W. C. Xue, X. Zeng, S. N. Zhang, H. S. Zhao, X. F. Zhao
Figure caption: The optical afterglow of GRB 221009A was observed using the ﹩{g}^{{\prime} }{{Vr}}^{{\prime} }{R}_{C}{i}^{{\prime} }{I}_{C}{z}^{{\prime} }﹩ filters and without a filter, with data points shown in the observer frame. The selected optical GCN data we use are represented by dots, and the GRANDMA data measurements and upper limits are indicated by larger stars and downward-pointing triangles (see Appendix). The red points within the stars indicate measurements made by professional observers, while black points represent observations made by KNC observers. Only magnitude measurements with at least a 3σ detection significance are included (the upper limits being given at 5σ significance), with uncertainty regions shown as shading. The measurements are not corrected for any extinction.
Paper: GRANDMA and HXMT Observations of GRB 221009A: The Standard Luminosity Afterglow of a Hyperluminous Gamma-Ray Burst—In Gedenken an David Alexander Kann
Authors: D. A. Kann, S. Agayeva, V. Aivazyan, S. Alishov, C. M. Andrade, S. Antier, A. Baransky, P. Bendjoya, Z. Benkhaldoun, S. Beradze, D. Berezin, M. Boër, E. Broens, S. Brunier, M. Bulla, O. Burkhonov, E. Burns, Y. Chen, Y. P. Chen, M. Conti, M. W. Coughlin, W. W. Cui, F. Daigne, B. Delaveau, H. A. R. Devillepoix, T. Dietrich, D. Dornic, F. Dubois, J.-G. Ducoin, E. Durand, P.-A. Duverne, H.-B. Eggenstein, S. Ehgamberdiev, A. Fouad, M. Freeberg, D. Froebrich, M. Y. Ge, S. Gervasoni, V. Godunova, P. Gokuldass, E. Gurbanov, D. W. Han, E. Hasanov, P. Hello, T. Hussenot-Desenonges, R. Inasaridze, A. Iskandar, N. Ismailov, A. Janati, T. Jegou du Laz, S. M. Jia, S. Karpov, A. Kaeouach, R. W. Kiendrebeogo, A. Klotz, R. Kneip, N. Kochiashvili, N. Kunert, A. Lekic, S. Leonini, C. K. Li, W. Li, X. B. Li, J. Y. Liao, L. Logie, F. J. Lu, J. Mao, D. Marchais, R. Ménard, D. Morris, R. Natsvlishvili, V. Nedora, K. Noonan, K. Noysena, N. B. Orange, P. T. H. Pang, H. W. Peng, C. Pellouin, J. Peloton, T. Pradier, O. Pyshna, Y. Rajabov, S. Rau, C. Rinner, J.-P. Rivet, F. D. Romanov, P. Rosi, V. A. Rupchandani, M. Serrau, A. Shokry, A. Simon, K. Smith, O. Sokoliuk, M. Soliman, L. M. Song, A. Takey, Y. Tillayev, L. M. Tinjaca Ramirez, I. Tosta e Melo, D. Turpin, A. de Ugarte Postigo, S. Vanaverbeke, V. Vasylenko, D. Vernet, Z. Vidadi, C. Wang, J. Wang, L. T. Wang, X. F. Wang, S. L. Xiong, Y. P. Xu, W. C. Xue, X. Zeng, S. N. Zhang, H. S. Zhao, X. F. Zhao
Figure caption: The NMMA observational data (GRANDMA data) and best-fit light curves of selected filters for the NMMA analysis using the SF11 extinction and the four employed jet structures. The X-ray bands are shown in microjanskys, and the rest of the bands are shown in AB magnitude.
Paper: GRANDMA and HXMT Observations of GRB 221009A: The Standard Luminosity Afterglow of a Hyperluminous Gamma-Ray Burst—In Gedenken an David Alexander Kann
Authors: D. A. Kann, S. Agayeva, V. Aivazyan, S. Alishov, C. M. Andrade, S. Antier, A. Baransky, P. Bendjoya, Z. Benkhaldoun, S. Beradze, D. Berezin, M. Boër, E. Broens, S. Brunier, M. Bulla, O. Burkhonov, E. Burns, Y. Chen, Y. P. Chen, M. Conti, M. W. Coughlin, W. W. Cui, F. Daigne, B. Delaveau, H. A. R. Devillepoix, T. Dietrich, D. Dornic, F. Dubois, J.-G. Ducoin, E. Durand, P.-A. Duverne, H.-B. Eggenstein, S. Ehgamberdiev, A. Fouad, M. Freeberg, D. Froebrich, M. Y. Ge, S. Gervasoni, V. Godunova, P. Gokuldass, E. Gurbanov, D. W. Han, E. Hasanov, P. Hello, T. Hussenot-Desenonges, R. Inasaridze, A. Iskandar, N. Ismailov, A. Janati, T. Jegou du Laz, S. M. Jia, S. Karpov, A. Kaeouach, R. W. Kiendrebeogo, A. Klotz, R. Kneip, N. Kochiashvili, N. Kunert, A. Lekic, S. Leonini, C. K. Li, W. Li, X. B. Li, J. Y. Liao, L. Logie, F. J. Lu, J. Mao, D. Marchais, R. Ménard, D. Morris, R. Natsvlishvili, V. Nedora, K. Noonan, K. Noysena, N. B. Orange, P. T. H. Pang, H. W. Peng, C. Pellouin, J. Peloton, T. Pradier, O. Pyshna, Y. Rajabov, S. Rau, C. Rinner, J.-P. Rivet, F. D. Romanov, P. Rosi, V. A. Rupchandani, M. Serrau, A. Shokry, A. Simon, K. Smith, O. Sokoliuk, M. Soliman, L. M. Song, A. Takey, Y. Tillayev, L. M. Tinjaca Ramirez, I. Tosta e Melo, D. Turpin, A. de Ugarte Postigo, S. Vanaverbeke, V. Vasylenko, D. Vernet, Z. Vidadi, C. Wang, J. Wang, L. T. Wang, X. F. Wang, S. L. Xiong, Y. P. Xu, W. C. Xue, X. Zeng, S. N. Zhang, H. S. Zhao, X. F. Zhao
Figure caption: Analysis of the SED. Top panel: fit to the uncorrected SED with an MW extinction model at z = 0, i.e., assuming no additional host-galaxy extinction. The fit is generally in agreement with the data, with the uvw1 data point being brighter than the model. Middle panel: fit to the SED after correcting it for SF11 foreground extinction and shifting it to z = 0.151. The correction leads to significant scatter, with the uvw1 now being clearly brighter than any fit, even one without additional host-galaxy extinction. The three extinction laws cannot be discerned from each other, but the potential bright uvw1 emission makes the SMC law the preferred one. There is still significant curvature, which implies additional significant host-galaxy extinction. Bottom panel: same as the middle panel but with RF09 foreground extinction. The SED remains very red, and very high host extinction is implied. Again, SMC extinction leads to the most physical solution, but all dust laws are in conflict with the bluest Swift UVOT detection.
Paper: Early Results from GLASS-JWST. XVIII. A First Morphological Atlas of the 1 < z < 5 Universe in the Rest-frame Optical
Authors: C. Jacobs, K. Glazebrook, A. Calabrò, T. Treu, T. Nannayakkara, T. Jones, E. Merlin, R. Abraham, A. R. H. Stevens, B. Vulcani, L. Yang, A. Bonchi, K. Boyett, M. Bradač, M. Castellano, A. Fontana, D. Marchesini, M. Malkan, C. Mason, T. Morishita, D. Paris, P. Santini, M. Trenti, X. Wang
Figure caption: Rest-frame gri RGB images of selected sources organized by redshift bin (indicated at bottom, increasing left to right) and mass bin (indicated at left, decreasing top to bottom). Each postage stamp is 3.″1 wide. Morphological classifications are indicated, where p = peculiar, e = elliptical, d = disk, and bd = bulge and disk.
Paper: Early Results from GLASS-JWST. XVIII. A First Morphological Atlas of the 1 < z < 5 Universe in the Rest-frame Optical
Authors: C. Jacobs, K. Glazebrook, A. Calabrò, T. Treu, T. Nannayakkara, T. Jones, E. Merlin, R. Abraham, A. R. H. Stevens, B. Vulcani, L. Yang, A. Bonchi, K. Boyett, M. Bradač, M. Castellano, A. Fontana, D. Marchesini, M. Malkan, C. Mason, T. Morishita, D. Paris, P. Santini, M. Trenti, X. Wang
Figure caption: Morphology by mass and redshift bin, with the fraction of sources in each of our broad morphological categories shown. “Disky” refers to the union of “disk” and “disk+bulge” classifications. The contribution from disk+bulge galaxies to the disky fraction is shown with dashed lines. Here we divide the sample into two mass bins with approximately equal numbers. The number of our 388 sources in each of the redshift bins is also given. Error bars indicate the multinomial statistical 1σ uncertainty, but they do not account for misclassification error.
Paper: Early Results from GLASS-JWST. XVIII. A First Morphological Atlas of the 1 < z < 5 Universe in the Rest-frame Optical
Authors: C. Jacobs, K. Glazebrook, A. Calabrò, T. Treu, T. Nannayakkara, T. Jones, E. Merlin, R. Abraham, A. R. H. Stevens, B. Vulcani, L. Yang, A. Bonchi, K. Boyett, M. Bradač, M. Castellano, A. Fontana, D. Marchesini, M. Malkan, C. Mason, T. Morishita, D. Paris, P. Santini, M. Trenti, X. Wang
Figure caption: RGB images of SDSS galaxies in SDSS gri bands (left) and simulated NIRCam observations at z = 0.83, z = 1.43, and z = 2.38 in gri analogs, per Table 1. The stellar masses (﹩\mathrm{log}{M}_{* }/{M}_{\odot }﹩) are indicated in orange. The SDSS images are 101″ on a side, while the NIRCam simulations are 8″; the physical dimensions are 54, 34, 25, and 52 kpc from top to bottom.
Paper: Early Results from GLASS-JWST. XVIII. A First Morphological Atlas of the 1 < z < 5 Universe in the Rest-frame Optical
Authors: C. Jacobs, K. Glazebrook, A. Calabrò, T. Treu, T. Nannayakkara, T. Jones, E. Merlin, R. Abraham, A. R. H. Stevens, B. Vulcani, L. Yang, A. Bonchi, K. Boyett, M. Bradač, M. Castellano, A. Fontana, D. Marchesini, M. Malkan, C. Mason, T. Morishita, D. Paris, P. Santini, M. Trenti, X. Wang
Figure caption: Morphological measurements of our sample, with Gini coefficient on the x-axis and asymmetry on the y-axis. Top: the Gini–A plane for SDSS, our sample and the HST comparison sample respectively, with all sources plotted in gray and the mean A and gini values indicated in color. Histograms for each sample are also shown. The rest-frame UV imaging has higher G and A, due to clumpier morphology than rest-frame optical. Bottom: our sample color coded by morphological classification, with ellipticals in red, disks in blue, and irregulars in green. The sources mass-matched with the HST sample are shown as filled shapes. Our morphological classifications are in broad agreement with the GA values.
Paper: Steeper Scattered Disks Buckle Faster
Authors: Alexander Zderic, Ann-Marie Madigan
Figure caption: Timescale of the inclination instability, t insta, as a function of semimajor axis distribution index, α. N = 400 and M disk = 10−3 M ⊕ for all simulations. The instability timescale monotonically decreases with increasing α. Jitter is added to reveal overlapping points.
Paper: Steeper Scattered Disks Buckle Faster
Authors: Alexander Zderic, Ann-Marie Madigan
Figure caption: Absolute value of the mean i b for three disks with different semimajor axis distribution indices, α, and identical N and M disk. We have truncated points after the linear stage of the instability to emphasize the growth rate differences. The timescale for the instability clearly decreases with increasing α (steeper density profiles).
Paper: Steeper Scattered Disks Buckle Faster
Authors: Alexander Zderic, Ann-Marie Madigan
Figure caption: Instability and precession timescale ratio, r, as a function of disk mass, M disk, calculated from our simulations. α is distinguished by color and marker. The critical r value determining the transition from stability (above) to instability (below) is shown with a gray band. We find that α ≤ 1 have similar disk mass requirements needing more than 20 M ⊕ to be unstable, while α > 1 require less mass to be unstable.
Paper: Steeper Scattered Disks Buckle Faster
Authors: Alexander Zderic, Ann-Marie Madigan
Figure caption: Box and whisker plot of the instability timescale normalized by the mean (top) and median (bottom) period within the disk. The median period properly detrends the data suggesting the that growth rate at fixed M disk and N is determined by the median period of an orbit in the disk.
Paper: A Luminous Dust-obscured Tidal Disruption Event Candidate in a Star-forming Galaxy at 42 Mpc
Authors: Christos Panagiotou, Kishalay De, Megan Masterson, Erin Kara, Michael Calzadilla, Anna-Christina Eilers, Danielle Frostig, Viraj Karambelkar, Mansi Kasliwal, Nathan Lourie, Aaron M. Meisner, Robert A. Simcoe, Robert Stein, Jeffry Zolkower
Figure caption: Multicolor light curves of WTP14adbjsh. Upper panels: image cutouts at the location of NGC 7392. The first three panels show the single-epoch NEOWISE image at the time of the observed peak of the IR flare in 2015, the unWISE reference image created from stacking AllWISE data from 2010 to 2011, and the difference image between the science and reference image, respectively. The fourth panel shows an archival optical composite gri image from PanSTARRS1. Lower panel: combined WISE (mid-IR) and All-sky Automated Survey for Supernovae (ASASSN; optical) host subtracted light curves of the flare. The error bars are not distinguishable due to their nominal small value. The left y-axis denotes the observed flux of the transient, while the right y-axis denotes the corresponding monochromatic luminosity for a wavelength of 4 μm. The ASASSN data were stacked in 15 day bins to improve the SNR, while the mid-IR light curve points correspond to individual visits from WISE separated by 6 months. The inset shows the optical PSF-flux measurements (without host subtraction) at the location of the nucleus from the PS1 catalog, demonstrating no evidence for an optical flare in the 5 yr leading up to the mid-IR transient.
Paper: A Luminous Dust-obscured Tidal Disruption Event Candidate in a Star-forming Galaxy at 42 Mpc
Authors: Christos Panagiotou, Kishalay De, Megan Masterson, Erin Kara, Michael Calzadilla, Anna-Christina Eilers, Danielle Frostig, Viraj Karambelkar, Mansi Kasliwal, Nathan Lourie, Aaron M. Meisner, Robert A. Simcoe, Robert Stein, Jeffry Zolkower
Figure caption: Upper panel: mid-IR bolometric luminosity (left axis) and total radiated energy (right axis) of WTP14adbjsh as a function of time, overplotted with a t −5/3 time-evolution dependence for the luminosity. Lower panel: the mid-IR color temperature (left axis) and effective radius (right axis) evolution of the transient. The low-level radius and temperature fluctuations in successive epochs during the post-peak fading are a result of the oscillating W1 flux (Figure 1) that are caused by uncorrected and systematic PSF-shape variations on this very bright transient (Section 2.1).