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V F Suleimanov - One of the best experts on this subject based on the ideXlab platform.
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relation between the x ray and optical luminosities in binary systems with accreting nonmagnetic white dwarfs
arXiv: High Energy Astrophysical Phenomena, 2014Co-Authors: M Revnivtsev, E V Filippova, V F SuleimanovAbstract:We investigate the relation between the optical (g-band) and X-ray (0.5-10 keV) luminosities of accreting nonmagnetic white dwarfs. According to the present-day counts of the populations of star systems in our Galaxy, these systems have the highest space density among the close binary systems with white dwarfs. We show that the dependence of the optical luminosity of accreting white dwarfs on their X-ray luminosity forms a fairly narrow one-Parameter Curve. The typical half-width of this Curve does not exceed 0.2-0.3 dex in optical and X-ray luminosities, which is essentially consistent with the amplitude of the aperiodic flux variability for these objects. At X-ray luminosities Lx~1e32 erg/sec or lower, the optical g-band luminosity of the accretion flow is shown to be related to its X-ray luminosity by a factor ~2-3. At even lower X-ray luminosities (Lx~1e30 erg/sec), the contribution from the photosphere of the white dwarf begins to dominate in the optical spectrum of the binary system and its optical brightness does not drop below Mg~13-14. Using the latter fact, we show that in current and planned X-ray sky surveys, the family of accreting nonmagnetic white dwarfs can be completely identified to the distance determined by the sensitivity of an optical sky survey in this region. For the Sloan Digital Sky Survey (SDSS) with a limiting sensitivity m_g~22.5, this distance is ~400-600 pc
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relation between the x ray and optical luminosities in binary systems with accreting nonmagnetic white dwarfs
Astronomy Letters, 2014Co-Authors: M Revnivtsev, E V Filippova, V F SuleimanovAbstract:We investigate the relation between the optical (g-band) and X-ray (0.5–10 keV) luminosities of accreting nonmagnetic white dwarfs. According to the present-day counts of the populations of star systems in our Galaxy, these systems have the highest space density among the close binary systems with white dwarfs. We show that the dependence of the optical luminosity of accreting white dwarfs on their X-ray luminosity forms a fairly narrow one-Parameter Curve. The typical half-width of this Curve does not exceed 0.2–0.3 dex in optical and X-ray luminosities, which is essentially consistent with the amplitude of the aperiodic flux variability for these objects. At X-ray luminosities Lx ∼ 1032 erg s−1 or lower, the optical g-band luminosity of the accretion flow is shown to be related to its X-ray luminosity by a factor ∼2–3. At even lower X-ray luminosities (Lx ≲ 1030 erg s−1), the contribution from the photosphere of the white dwarf begins to dominate in the optical spectrum of the binary system and its optical brightness does not drop below Mg ∼ 13–14. Using the latter fact, we show that in current and planned X-ray sky surveys, the family of accreting nonmagnetic white dwarfs can be completely identified to the distance determined by the sensitivity of an optical sky survey in this region. For the Sloan Digital Sky Survey (SDSS) with a limiting sensitivity mg ∼ 22.5, this distance is ∼400–600 pc.
E V Filippova - One of the best experts on this subject based on the ideXlab platform.
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relation between the x ray and optical luminosities in binary systems with accreting nonmagnetic white dwarfs
arXiv: High Energy Astrophysical Phenomena, 2014Co-Authors: M Revnivtsev, E V Filippova, V F SuleimanovAbstract:We investigate the relation between the optical (g-band) and X-ray (0.5-10 keV) luminosities of accreting nonmagnetic white dwarfs. According to the present-day counts of the populations of star systems in our Galaxy, these systems have the highest space density among the close binary systems with white dwarfs. We show that the dependence of the optical luminosity of accreting white dwarfs on their X-ray luminosity forms a fairly narrow one-Parameter Curve. The typical half-width of this Curve does not exceed 0.2-0.3 dex in optical and X-ray luminosities, which is essentially consistent with the amplitude of the aperiodic flux variability for these objects. At X-ray luminosities Lx~1e32 erg/sec or lower, the optical g-band luminosity of the accretion flow is shown to be related to its X-ray luminosity by a factor ~2-3. At even lower X-ray luminosities (Lx~1e30 erg/sec), the contribution from the photosphere of the white dwarf begins to dominate in the optical spectrum of the binary system and its optical brightness does not drop below Mg~13-14. Using the latter fact, we show that in current and planned X-ray sky surveys, the family of accreting nonmagnetic white dwarfs can be completely identified to the distance determined by the sensitivity of an optical sky survey in this region. For the Sloan Digital Sky Survey (SDSS) with a limiting sensitivity m_g~22.5, this distance is ~400-600 pc
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relation between the x ray and optical luminosities in binary systems with accreting nonmagnetic white dwarfs
Astronomy Letters, 2014Co-Authors: M Revnivtsev, E V Filippova, V F SuleimanovAbstract:We investigate the relation between the optical (g-band) and X-ray (0.5–10 keV) luminosities of accreting nonmagnetic white dwarfs. According to the present-day counts of the populations of star systems in our Galaxy, these systems have the highest space density among the close binary systems with white dwarfs. We show that the dependence of the optical luminosity of accreting white dwarfs on their X-ray luminosity forms a fairly narrow one-Parameter Curve. The typical half-width of this Curve does not exceed 0.2–0.3 dex in optical and X-ray luminosities, which is essentially consistent with the amplitude of the aperiodic flux variability for these objects. At X-ray luminosities Lx ∼ 1032 erg s−1 or lower, the optical g-band luminosity of the accretion flow is shown to be related to its X-ray luminosity by a factor ∼2–3. At even lower X-ray luminosities (Lx ≲ 1030 erg s−1), the contribution from the photosphere of the white dwarf begins to dominate in the optical spectrum of the binary system and its optical brightness does not drop below Mg ∼ 13–14. Using the latter fact, we show that in current and planned X-ray sky surveys, the family of accreting nonmagnetic white dwarfs can be completely identified to the distance determined by the sensitivity of an optical sky survey in this region. For the Sloan Digital Sky Survey (SDSS) with a limiting sensitivity mg ∼ 22.5, this distance is ∼400–600 pc.
M Revnivtsev - One of the best experts on this subject based on the ideXlab platform.
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relation between the x ray and optical luminosities in binary systems with accreting nonmagnetic white dwarfs
arXiv: High Energy Astrophysical Phenomena, 2014Co-Authors: M Revnivtsev, E V Filippova, V F SuleimanovAbstract:We investigate the relation between the optical (g-band) and X-ray (0.5-10 keV) luminosities of accreting nonmagnetic white dwarfs. According to the present-day counts of the populations of star systems in our Galaxy, these systems have the highest space density among the close binary systems with white dwarfs. We show that the dependence of the optical luminosity of accreting white dwarfs on their X-ray luminosity forms a fairly narrow one-Parameter Curve. The typical half-width of this Curve does not exceed 0.2-0.3 dex in optical and X-ray luminosities, which is essentially consistent with the amplitude of the aperiodic flux variability for these objects. At X-ray luminosities Lx~1e32 erg/sec or lower, the optical g-band luminosity of the accretion flow is shown to be related to its X-ray luminosity by a factor ~2-3. At even lower X-ray luminosities (Lx~1e30 erg/sec), the contribution from the photosphere of the white dwarf begins to dominate in the optical spectrum of the binary system and its optical brightness does not drop below Mg~13-14. Using the latter fact, we show that in current and planned X-ray sky surveys, the family of accreting nonmagnetic white dwarfs can be completely identified to the distance determined by the sensitivity of an optical sky survey in this region. For the Sloan Digital Sky Survey (SDSS) with a limiting sensitivity m_g~22.5, this distance is ~400-600 pc
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relation between the x ray and optical luminosities in binary systems with accreting nonmagnetic white dwarfs
Astronomy Letters, 2014Co-Authors: M Revnivtsev, E V Filippova, V F SuleimanovAbstract:We investigate the relation between the optical (g-band) and X-ray (0.5–10 keV) luminosities of accreting nonmagnetic white dwarfs. According to the present-day counts of the populations of star systems in our Galaxy, these systems have the highest space density among the close binary systems with white dwarfs. We show that the dependence of the optical luminosity of accreting white dwarfs on their X-ray luminosity forms a fairly narrow one-Parameter Curve. The typical half-width of this Curve does not exceed 0.2–0.3 dex in optical and X-ray luminosities, which is essentially consistent with the amplitude of the aperiodic flux variability for these objects. At X-ray luminosities Lx ∼ 1032 erg s−1 or lower, the optical g-band luminosity of the accretion flow is shown to be related to its X-ray luminosity by a factor ∼2–3. At even lower X-ray luminosities (Lx ≲ 1030 erg s−1), the contribution from the photosphere of the white dwarf begins to dominate in the optical spectrum of the binary system and its optical brightness does not drop below Mg ∼ 13–14. Using the latter fact, we show that in current and planned X-ray sky surveys, the family of accreting nonmagnetic white dwarfs can be completely identified to the distance determined by the sensitivity of an optical sky survey in this region. For the Sloan Digital Sky Survey (SDSS) with a limiting sensitivity mg ∼ 22.5, this distance is ∼400–600 pc.
Michael A. Mancini - One of the best experts on this subject based on the ideXlab platform.
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Calculated Max and EC50 Responses of AIS GSF Cell Lines.
2013Co-Authors: Adam T. Szafra, Sea Hartig, Ivan P. Uray, Maria Szwarc, Yuqing She, Sanjay N. Mediwala, Jennife Ell, Michael J. Mcphaul, Michael A. ManciniAbstract:Values calculated by applying the 4-Parameter Curve fit algorithm available in SigmaPlot to multiple replicate experiments. All data are presented as absolute numerical measurements.Calculated maximal responses from AR HCA.EC50 values for Nuclear Translocation, Hyperspeckling and Total AR increase after stimulation with three AR agonists (DHT, Mibolerone and R1881) in GSF from AIS patients with AR mutations F764L, R840C and P766S. EC50 represents the nM concentration of agonist that provokes a response halfway between the baseline and maximal induction. Maximal response achieved with each agonist for each HTM Parameter is expressed as % signal present in the nucleus for Nuclear Translocation, as fold-induction from time point 0 for Hyperspeckling and Total AR content.
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Calculated Maximal and EC50 Responses of AIS Mutations in HeLa Cells.
2013Co-Authors: Adam T. Szafra, Sea Hartig, Ivan P. Uray, Maria Szwarc, Yuqing She, Sanjay N. Mediwala, Jennife Ell, Michael J. Mcphaul, Michael A. ManciniAbstract:Values calculated by applying the 4-Parameter Curve fit algorithm available in SigmaPlot to multiple replicate experiments and represent Mean±S.E.M. All data are presented as absolute numerical measurements.Calculated maximal responses from AR HCA. EC50 values are presented for Nuclear Translocation, Hyperspeckling and Transcriptional Activity after stimulation with three AR agonists (DHT, Mibolerone and R1881) in HeLa transfected with wild type AR, AR-F764L, AR-R840C and AR-P766S. EC50 represents the nM concentration of agonist that provokes a response halfway between the baseline and maximal induction. Maximal response achieved with each agonist for each HTM Parameter is expressed as % signal present in the nucleus for Nuclear Translocation, as fold-induction from time point 0 for Hyperspeckling and Transcriptional Activity.
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Calculated Max and EC50 Responses of Normal GSF Cell Lines.
2013Co-Authors: Adam T. Szafra, Sea Hartig, Ivan P. Uray, Maria Szwarc, Yuqing She, Sanjay N. Mediwala, Jennife Ell, Michael J. Mcphaul, Michael A. ManciniAbstract:Values calculated by applying the 4-Parameter Curve fit algorithm available in SigmaPlot to multiple replicate experiments. For individual cell lines, all data are presented as absolute numerical measurements. For the average normal response, nuclear translocation is reported as the percentage point change from untreated samples whereas hyperspeckling and total AR is reported as fold change from untreated samples.Calculated maximal responses from AR HCA. EC50 values for Nuclear Translocation, Hyperspeckling and Total AR increase after stimulation with three AR agonists (DHT, Mibolerone and R1881) in GSF from 6 normal individuals (M6382, L7728, M7118, A4676, S8558, B8906). EC50 represents the nM concentration of agonist that provokes a response halfway between the baseline and maximal induction. Maximal response achieved with each agonist for each HTM Parameter is expressed as % signal present in the nucleus for Nuclear Translocation, as fold-induction from time point 0 for Hyperspeckling and Total AR content.
Adam T. Szafra - One of the best experts on this subject based on the ideXlab platform.
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Calculated Max and EC50 Responses of AIS GSF Cell Lines.
2013Co-Authors: Adam T. Szafra, Sea Hartig, Ivan P. Uray, Maria Szwarc, Yuqing She, Sanjay N. Mediwala, Jennife Ell, Michael J. Mcphaul, Michael A. ManciniAbstract:Values calculated by applying the 4-Parameter Curve fit algorithm available in SigmaPlot to multiple replicate experiments. All data are presented as absolute numerical measurements.Calculated maximal responses from AR HCA.EC50 values for Nuclear Translocation, Hyperspeckling and Total AR increase after stimulation with three AR agonists (DHT, Mibolerone and R1881) in GSF from AIS patients with AR mutations F764L, R840C and P766S. EC50 represents the nM concentration of agonist that provokes a response halfway between the baseline and maximal induction. Maximal response achieved with each agonist for each HTM Parameter is expressed as % signal present in the nucleus for Nuclear Translocation, as fold-induction from time point 0 for Hyperspeckling and Total AR content.
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Calculated Maximal and EC50 Responses of AIS Mutations in HeLa Cells.
2013Co-Authors: Adam T. Szafra, Sea Hartig, Ivan P. Uray, Maria Szwarc, Yuqing She, Sanjay N. Mediwala, Jennife Ell, Michael J. Mcphaul, Michael A. ManciniAbstract:Values calculated by applying the 4-Parameter Curve fit algorithm available in SigmaPlot to multiple replicate experiments and represent Mean±S.E.M. All data are presented as absolute numerical measurements.Calculated maximal responses from AR HCA. EC50 values are presented for Nuclear Translocation, Hyperspeckling and Transcriptional Activity after stimulation with three AR agonists (DHT, Mibolerone and R1881) in HeLa transfected with wild type AR, AR-F764L, AR-R840C and AR-P766S. EC50 represents the nM concentration of agonist that provokes a response halfway between the baseline and maximal induction. Maximal response achieved with each agonist for each HTM Parameter is expressed as % signal present in the nucleus for Nuclear Translocation, as fold-induction from time point 0 for Hyperspeckling and Transcriptional Activity.
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Calculated Max and EC50 Responses of Normal GSF Cell Lines.
2013Co-Authors: Adam T. Szafra, Sea Hartig, Ivan P. Uray, Maria Szwarc, Yuqing She, Sanjay N. Mediwala, Jennife Ell, Michael J. Mcphaul, Michael A. ManciniAbstract:Values calculated by applying the 4-Parameter Curve fit algorithm available in SigmaPlot to multiple replicate experiments. For individual cell lines, all data are presented as absolute numerical measurements. For the average normal response, nuclear translocation is reported as the percentage point change from untreated samples whereas hyperspeckling and total AR is reported as fold change from untreated samples.Calculated maximal responses from AR HCA. EC50 values for Nuclear Translocation, Hyperspeckling and Total AR increase after stimulation with three AR agonists (DHT, Mibolerone and R1881) in GSF from 6 normal individuals (M6382, L7728, M7118, A4676, S8558, B8906). EC50 represents the nM concentration of agonist that provokes a response halfway between the baseline and maximal induction. Maximal response achieved with each agonist for each HTM Parameter is expressed as % signal present in the nucleus for Nuclear Translocation, as fold-induction from time point 0 for Hyperspeckling and Total AR content.
