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3 results on '"Krimm HA"'

1. Swift Monitoring of NGC 4151: Evidence for a Second X-Ray/UV Reprocessing

Author

Edelson, R, Edelson, R, Gelbord, J, Cackett, E, Connolly, S, Done, C, Fausnaugh, M, Gardner, E, Gehrels, N, Goad, M, Horne, K, McHardy, I, Peterson, BM, Vaughan, S, Vestergaard, M, Breeveld, A, Barth, AJ, Bentz, M, Bottorff, M, Brandt, WN, Crawford, SM, Dalla Bontà, E, Emmanoulopoulos, D, Evans, P, Jaimes, RF, Filippenko, AV, Ferland, G, Grupe, D, Joner, M, Kennea, J, Korista, KT, Krimm, HA, Kriss, G, Leonard, DC, Mathur, S, Netzer, H, Nousek, J, Page, K, Romero-Colmenero, E, Siegel, M, Starkey, DA, Treu, T, Vogler, HA, Winkler, H, Zheng, W, Edelson, R, Edelson, R, Gelbord, J, Cackett, E, Connolly, S, Done, C, Fausnaugh, M, Gardner, E, Gehrels, N, Goad, M, Horne, K, McHardy, I, Peterson, BM, Vaughan, S, Vestergaard, M, Breeveld, A, Barth, AJ, Bentz, M, Bottorff, M, Brandt, WN, Crawford, SM, Dalla Bontà, E, Emmanoulopoulos, D, Evans, P, Jaimes, RF, Filippenko, AV, Ferland, G, Grupe, D, Joner, M, Kennea, J, Korista, KT, Krimm, HA, Kriss, G, Leonard, DC, Mathur, S, Netzer, H, Nousek, J, Page, K, Romero-Colmenero, E, Siegel, M, Starkey, DA, Treu, T, Vogler, HA, Winkler, H, and Zheng, W

Abstract

Swift monitoring of NGC 4151 with an ∼6 hr sampling over a total of 69 days in early 2016 is used to construct light curves covering five bands in the X-rays (0.3-50 keV) and six in the ultraviolet (UV)/optical (1900-5500 Å). The three hardest X-ray bands (>2.5 keV) are all strongly correlated with no measurable interband lag, while the two softer bands show lower variability and weaker correlations. The UV/optical bands are significantly correlated with the X-rays, lagging ∼3-4 days behind the hard X-rays. The variability within the UV/optical bands is also strongly correlated, with the UV appearing to lead the optical by ∼0.5-1 days. This combination of ≳3 day lags between the X-rays and UV and ≲1 day lags within the UV/optical appears to rule out the "lamp-post" reprocessing model in which a hot, X-ray emitting corona directly illuminates the accretion disk, which then reprocesses the energy in the UV/optical. Instead, these results appear consistent with the Gardner & Done picture in which two separate reprocessings occur: first, emission from the corona illuminates an extreme-UV-emitting toroidal component that shields the disk from the corona; this then heats the extreme-UV component, which illuminates the disk and drives its variability.

Published
2017

2. Swift Monitoring of NGC 4151: Evidence for a Second X-Ray/UV Reprocessing

Author

Edelson, R, Edelson, R, Gelbord, J, Cackett, E, Connolly, S, Done, C, Fausnaugh, M, Gardner, E, Gehrels, N, Goad, M, Horne, K, McHardy, I, Peterson, BM, Vaughan, S, Vestergaard, M, Breeveld, A, Barth, AJ, Bentz, M, Bottorff, M, Brandt, WN, Crawford, SM, Dalla Bontà, E, Emmanoulopoulos, D, Evans, P, Jaimes, RF, Filippenko, AV, Ferland, G, Grupe, D, Joner, M, Kennea, J, Korista, KT, Krimm, HA, Kriss, G, Leonard, DC, Mathur, S, Netzer, H, Nousek, J, Page, K, Romero-Colmenero, E, Siegel, M, Starkey, DA, Treu, T, Vogler, HA, Winkler, H, Zheng, W, Edelson, R, Edelson, R, Gelbord, J, Cackett, E, Connolly, S, Done, C, Fausnaugh, M, Gardner, E, Gehrels, N, Goad, M, Horne, K, McHardy, I, Peterson, BM, Vaughan, S, Vestergaard, M, Breeveld, A, Barth, AJ, Bentz, M, Bottorff, M, Brandt, WN, Crawford, SM, Dalla Bontà, E, Emmanoulopoulos, D, Evans, P, Jaimes, RF, Filippenko, AV, Ferland, G, Grupe, D, Joner, M, Kennea, J, Korista, KT, Krimm, HA, Kriss, G, Leonard, DC, Mathur, S, Netzer, H, Nousek, J, Page, K, Romero-Colmenero, E, Siegel, M, Starkey, DA, Treu, T, Vogler, HA, Winkler, H, and Zheng, W

Abstract

Swift monitoring of NGC 4151 with an ∼6 hr sampling over a total of 69 days in early 2016 is used to construct light curves covering five bands in the X-rays (0.3-50 keV) and six in the ultraviolet (UV)/optical (1900-5500 Å). The three hardest X-ray bands (>2.5 keV) are all strongly correlated with no measurable interband lag, while the two softer bands show lower variability and weaker correlations. The UV/optical bands are significantly correlated with the X-rays, lagging ∼3-4 days behind the hard X-rays. The variability within the UV/optical bands is also strongly correlated, with the UV appearing to lead the optical by ∼0.5-1 days. This combination of ≳3 day lags between the X-rays and UV and ≲1 day lags within the UV/optical appears to rule out the "lamp-post" reprocessing model in which a hot, X-ray emitting corona directly illuminates the accretion disk, which then reprocesses the energy in the UV/optical. Instead, these results appear consistent with the Gardner & Done picture in which two separate reprocessings occur: first, emission from the corona illuminates an extreme-UV-emitting toroidal component that shields the disk from the corona; this then heats the extreme-UV component, which illuminates the disk and drives its variability.

Published
2017

3. The swift gamma-ray burst mission

Author

Gehrels, N, Chincarini, G, Giommi, P, Mason, K, Nousek, J, Wells, A, White, N, Barthelmy, S, Burrows, D, Cominsky, L, Hurley, K, Marshall, F, Meszaros, P, Roming, P, Angelini, L, Barbier, L, Belloni, T, Boyd, P, Campana, S, Caraveo, P, Chester, M, Citterio, O, Cline, T, Cropper, M, Cummings, J, Dean, A, Feigelson, E, Fenimore, E, Frail, D, Fruchter, A, Garmire, G, Gendreau, K, Ghisellini, G, Greiner, J, Hill, J, Hunsberger, S, Krimm, H, Kulkarni, S, Kumar, P, Lebrun, F, Lloyd Ronning, N, Markwardt, C, Mattson, B, Mushotzky, R, Norris, J, Paczynski, B, Palmer, D, Park, H, Parsons, A, Paul, J, Rees, M, Reynolds, C, Rhoads, J, Sasseen, T, Schaefer, B, Short, A, Smale, A, Smith, I, Stella, L, Still, M, Tagliaferri, G, Takahashi, T, Tashiro, M, Townsley, L, Tueller, J, Turner, M, Vietri, M, Voges, W, Ward, M, Willingale, R, Zerbi, F, Zhang, W, Mason, KO, Nousek, JA, Wells, AA, White, NE, Barthelmy, SD, Burrows, DN, Cominsky, LR, Hurley, KC, Marshall, FE, Roming, PWA, Barbier, LM, Boyd, PT, Caraveo, PA, Chester, MM, Cline, TL, Cropper, MS, Cummings, JR, Dean, AJ, Feigelson, ED, Fenimore, EE, Frail, DA, Fruchter, AS, Garmire, GP, Hill, JE, Hunsberger, SD, Krimm, HA, Kulkarni, SR, Lloyd Ronning, NM, Markwardt, CB, Mattson, BJ, Mushotzky, RF, Norris, JP, Palmer, DM, Park, HS, Parsons, AM, Rees, MJ, Reynolds, CS, Rhoads, JE, Sasseen, TP, Schaefer, BE, Short, AT, Smale, AP, Smith, IA, Townsley, LK, Turner, MJL, Ward, MJ, Zerbi, FM, Zhang, WW, CHINCARINI, GUIDO, Gehrels, N, Chincarini, G, Giommi, P, Mason, K, Nousek, J, Wells, A, White, N, Barthelmy, S, Burrows, D, Cominsky, L, Hurley, K, Marshall, F, Meszaros, P, Roming, P, Angelini, L, Barbier, L, Belloni, T, Boyd, P, Campana, S, Caraveo, P, Chester, M, Citterio, O, Cline, T, Cropper, M, Cummings, J, Dean, A, Feigelson, E, Fenimore, E, Frail, D, Fruchter, A, Garmire, G, Gendreau, K, Ghisellini, G, Greiner, J, Hill, J, Hunsberger, S, Krimm, H, Kulkarni, S, Kumar, P, Lebrun, F, Lloyd Ronning, N, Markwardt, C, Mattson, B, Mushotzky, R, Norris, J, Paczynski, B, Palmer, D, Park, H, Parsons, A, Paul, J, Rees, M, Reynolds, C, Rhoads, J, Sasseen, T, Schaefer, B, Short, A, Smale, A, Smith, I, Stella, L, Still, M, Tagliaferri, G, Takahashi, T, Tashiro, M, Townsley, L, Tueller, J, Turner, M, Vietri, M, Voges, W, Ward, M, Willingale, R, Zerbi, F, Zhang, W, Mason, KO, Nousek, JA, Wells, AA, White, NE, Barthelmy, SD, Burrows, DN, Cominsky, LR, Hurley, KC, Marshall, FE, Roming, PWA, Barbier, LM, Boyd, PT, Caraveo, PA, Chester, MM, Cline, TL, Cropper, MS, Cummings, JR, Dean, AJ, Feigelson, ED, Fenimore, EE, Frail, DA, Fruchter, AS, Garmire, GP, Hill, JE, Hunsberger, SD, Krimm, HA, Kulkarni, SR, Lloyd Ronning, NM, Markwardt, CB, Mattson, BJ, Mushotzky, RF, Norris, JP, Palmer, DM, Park, HS, Parsons, AM, Rees, MJ, Reynolds, CS, Rhoads, JE, Sasseen, TP, Schaefer, BE, Short, AT, Smale, AP, Smith, IA, Townsley, LK, Turner, MJL, Ward, MJ, Zerbi, FM, Zhang, WW, and CHINCARINI, GUIDO

Abstract

The Swift mission, scheduled for launch in 2004, is a multiwavelength observatory for gamma-ray burst (GRB) astronomy. It is a first-of-its-kind autonomous rapid-slewing satellite for transient astronomy and pioneers the way for future rapid-reaction and multiwavelength missions. It will be far more powerful than any previous GRB mission, observing more than 100 bursts yr 1 and performing detailed X-ray and UV/optical afterglow observations spanning timescales from 1 minute to several days after the burst. The objectives are to (1) determine the origin of GRBs, (2) classify GRBs and search for new types, (3) study the interaction of the ultrarelativistic outflows of GRBs with their surrounding medium, and (4) use GRBs to study the early universe out to z>10. The mission is being developed by a NASA-led international collaboration. It will carry three instruments: a newgeneration wide-field gamma-ray (15–150 keV) detector that will detect bursts, calculate 10–40 positions, and trigger autonomous spacecraft slews; a narrow-field X-ray telescope that will give 500 positions and perform spectroscopy in the 0.2–10 keV band; and a narrow-field UV/optical telescope that will operate in the 170– 600 nm band and provide 0B3 positions and optical finding charts. Redshift determinations will be made for most bursts. In addition to the primary GRB science, the mission will perform a hard X-ray survey to a sensitivity of 1 mcrab ( 2 ; 10 11 ergs cm 2 s 1 in the 15–150 keV band), more than an order of magnitude better than HEAO 1 A-4. A flexible data and operations system will allow rapid follow-up observations of all types of high-energy transients, with rapid data downlink and uplink available through the NASA TDRSS system. Swift transient data will be rapidly distributed to the astronomical community, and all interested observers are encouraged to participate in follow-up measurements. A Guest Investigator program for the mission will provide funding for community involvement.

Published
2004

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