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Paper: A Disintegrating Rocky World Shrouded in Dust and Gas: Mid-infrared Observations of K2-22 b Using JWST
Authors: Nick Tusay, Jason T. Wright, Thomas G. Beatty, Steve Desch, Knicole Colón, Tushar Mittal, Hugh P. Osborn, Beatriz Campos Estrada, James E. Owen, Jessica Libby-Roberts, Arvind F. Gupta, Brad Foley, Erik Meier Valdés, Daniel J. Stevens, Ashley Herbst
Figure caption: Gas opacities of rock and ice vapor overlaid with the MIRI data. The two most theoretically plausible species with significant mid-infrared features that are expected from typical mantle material are shown: MgO and SiO (R. A. Booth et al. 2023). These poorly fit the data, suggesting that these gases are not detected in the MIRI data. Many different ice species, binned to the same resolution as the spectral data, were considered from the DACE database. The best-fitting gas models are NO, and CO2 to explain the short-wavelength features from 4.4 to 5.3 μm.
Paper: A Disintegrating Rocky World Shrouded in Dust and Gas: Mid-infrared Observations of K2-22 b Using JWST
Authors: Nick Tusay, Jason T. Wright, Thomas G. Beatty, Steve Desch, Knicole Colón, Tushar Mittal, Hugh P. Osborn, Beatriz Campos Estrada, James E. Owen, Jessica Libby-Roberts, Arvind F. Gupta, Brad Foley, Erik Meier Valdés, Daniel J. Stevens, Ashley Herbst
Figure caption: Opacities calculated from optical properties of solid dust species using Mie scattering theory with an effective dust grain size of 1 μm for a power-law (p = 0.875) distribution of dust grains. Representative models for core, mantle, and crust mineralogy are included. This spectrum disfavors purely featureless iron compounds indicative of a bare core. None of these solid dust opacities simultaneously account for all the features in the spectrum, particularly falling short of describing the feature around 5 μm.
Paper: A Disintegrating Rocky World Shrouded in Dust and Gas: Mid-infrared Observations of K2-22 b Using JWST
Authors: Nick Tusay, Jason T. Wright, Thomas G. Beatty, Steve Desch, Knicole Colón, Tushar Mittal, Hugh P. Osborn, Beatriz Campos Estrada, James E. Owen, Jessica Libby-Roberts, Arvind F. Gupta, Brad Foley, Erik Meier Valdés, Daniel J. Stevens, Ashley Herbst
Figure caption: Time-averaged stellar spectrum with flux outliers removed. The turnover below 5 μm is due to reduced throughput. A sliding window of nine channels was used to identify points with a greater than 3σ deviation from its neighbors. Red “x” points are the outliers that were removed.
Paper: A Disintegrating Rocky World Shrouded in Dust and Gas: Mid-infrared Observations of K2-22 b Using JWST
Authors: Nick Tusay, Jason T. Wright, Thomas G. Beatty, Steve Desch, Knicole Colón, Tushar Mittal, Hugh P. Osborn, Beatriz Campos Estrada, James E. Owen, Jessica Libby-Roberts, Arvind F. Gupta, Brad Foley, Erik Meier Valdés, Daniel J. Stevens, Ashley Herbst
Figure caption: Two independent reductions of the MIRI LRS data for transit 4 agree within their uncertainties. Shown are our fiducial Eureka! results (Appendix A.1) and the results from a reduction using the Pegasus pipeline (Appendix A.2), plotted with their associated 1σ uncertainties at a constant spectral resolution of R = 17. Both reductions agree on the overall shape of the transmission spectrum and are consistent with each other to within 1σ.
Paper: A Disintegrating Rocky World Shrouded in Dust and Gas: Mid-infrared Observations of K2-22 b Using JWST
Authors: Nick Tusay, Jason T. Wright, Thomas G. Beatty, Steve Desch, Knicole Colón, Tushar Mittal, Hugh P. Osborn, Beatriz Campos Estrada, James E. Owen, Jessica Libby-Roberts, Arvind F. Gupta, Brad Foley, Erik Meier Valdés, Daniel J. Stevens, Ashley Herbst
Figure caption: MIRI verification image of K2-22 and its smaller companion star, at ∼2″ separation. The direction of dispersion (DOD) is included as well, showing enough separation between the binary that contamination is minimal. The DOD is ∼175∘ east of north.
Paper: A Disintegrating Rocky World Shrouded in Dust and Gas: Mid-infrared Observations of K2-22 b Using JWST
Authors: Nick Tusay, Jason T. Wright, Thomas G. Beatty, Steve Desch, Knicole Colón, Tushar Mittal, Hugh P. Osborn, Beatriz Campos Estrada, James E. Owen, Jessica Libby-Roberts, Arvind F. Gupta, Brad Foley, Erik Meier Valdés, Daniel J. Stevens, Ashley Herbst
Figure caption: MIRI LRS lightcurves for all four transit observations listed in Tables 1 and 2 for combined light of the spectral channels up to 8 μm. The unbinned data (at a cadence of 72 s) are grayed out in the background. The blue points are binned to a time resolution of 8 minutes. The red line is a second-order polynomial fit to transit 4 and scaled to the best-fit value in each window. Multiple transit models were fit, including the original K2 lightcurve, a skewed Gaussian, and a boxcar, with no significant difference in the overall depth or resulting spectrum. The 46 minute transit duration calculated by R. Sanchis-Ojeda et al. (2015) is included as vertical gray dashed lines for reference. The uncertainties in the data points as reported by Eureka! were inflated to match the actual standard deviation in the baseline flux.
Paper: A Disintegrating Rocky World Shrouded in Dust and Gas: Mid-infrared Observations of K2-22 b Using JWST
Authors: Nick Tusay, Jason T. Wright, Thomas G. Beatty, Steve Desch, Knicole Colón, Tushar Mittal, Hugh P. Osborn, Beatriz Campos Estrada, James E. Owen, Jessica Libby-Roberts, Arvind F. Gupta, Brad Foley, Erik Meier Valdés, Daniel J. Stevens, Ashley Herbst
Figure caption: Calculated ΔBIC values for select solid mineralogy opacities noted in Section 3.1 and shown in Figure 3 against a flat line as compared with our resulting spectrum at wavelengths < 8 μm. The top four models shown here, quartz (SiO2 [s]), olivine ((MgFe)2SiO4 [s]), enstatite (MgSiO3 [s]), and forsterite (Mg2SiO4 [s]), represent likely crust/mantle minerals. The bottom three, iron (Fe [s]), iron sulfide (FeS [s]), and iron oxide (FeO [s]), represent likely core minerals. We used two parameters to scale and offset the mineralogy models, and one parameter for the flat line. These ΔBIC values show that the spectrum data are more consistent with mantle mineralogy than either a flat spectrum or iron-dominant mineralogy. The different colored bars are a qualitative comparison of the results; negative values are shown in red, positive values below three are colored orange, and those above three are green.
Paper: A Disintegrating Rocky World Shrouded in Dust and Gas: Mid-infrared Observations of K2-22 b Using JWST
Authors: Nick Tusay, Jason T. Wright, Thomas G. Beatty, Steve Desch, Knicole Colón, Tushar Mittal, Hugh P. Osborn, Beatriz Campos Estrada, James E. Owen, Jessica Libby-Roberts, Arvind F. Gupta, Brad Foley, Erik Meier Valdés, Daniel J. Stevens, Ashley Herbst
Figure caption: Top: measured depth using the transit model as a fixed-duration sliding window across the combined-light time series for each observation up to 8 μm. This shows that there is some variation in the normalized flux for each transit, possibly due to systematics from MIRI. The most significant measurement occurs at the predicted transit center time of the fourth transit window, while low-significance measurements in transit windows 2 and 3 correspond to those reported in Section 3. Bottom: histogram of depth measurements (blue) at all times outside 1.5× the 46 minute duration of each transit window, i.e., “elsewhere” in the observations. The stand-alone observations, 1 and 2, show distinctly increased uncertainties and are thus treated separately from the full phase curve. The standard deviations in the distributions are ≲1.1× the calculated depth uncertainty, suggesting minimal effects from red noise. The red dashed line shows the measured depth at the center time of the fourth transit window for comparison.
Paper: A Disintegrating Rocky World Shrouded in Dust and Gas: Mid-infrared Observations of K2-22 b Using JWST
Authors: Nick Tusay, Jason T. Wright, Thomas G. Beatty, Steve Desch, Knicole Colón, Tushar Mittal, Hugh P. Osborn, Beatriz Campos Estrada, James E. Owen, Jessica Libby-Roberts, Arvind F. Gupta, Brad Foley, Erik Meier Valdés, Daniel J. Stevens, Ashley Herbst
Figure caption: A standard assessment of the residuals of the model fit to the lightcurve for transit 4 using the combined light of the MIRI spectral channels up to 8 μm. The blue line shows the rms of the residuals of the transit model fit to the data for different bin sizes. The unbinned data were taken with a cadence of 72 s, providing roughly 38 points across the assumed average transit duration. The orange line shows how our adopted single measurement uncertainty would scale as white noise as the data are binned up. The uncertainties in the data points as reported by Eureka! were inflated by a factor to match the actual standard deviation in the baseline flux for more conservatively accurate error estimates while preserving variations in the measurements.
Paper: A Disintegrating Rocky World Shrouded in Dust and Gas: Mid-infrared Observations of K2-22 b Using JWST
Authors: Nick Tusay, Jason T. Wright, Thomas G. Beatty, Steve Desch, Knicole Colón, Tushar Mittal, Hugh P. Osborn, Beatriz Campos Estrada, James E. Owen, Jessica Libby-Roberts, Arvind F. Gupta, Brad Foley, Erik Meier Valdés, Daniel J. Stevens, Ashley Herbst
Figure caption: MIRI spectra during all four expected transits using the second-degree transit model from transit 4, scaled to the optimal depth in each channel for each transit. Top: individual spectra during each transit window. The red dashed line marks the overall transit depth in transit 4. The purple dashed line indicates the overall transit depth in each observation as measured from the white-light lightcurves. The white-light time series of transit 4 shows a clear signal, while the others do not (see Figure C1). However, the most or second most significant detections in transit 1, transit 2, and transit 3 are in the 4.5 and 5.1 μm channels, supporting the reality of these narrow features observed at modest significance in transit 4. Bottom: combined spectra of all four transits. The 4.5 and 5.1 μm features are clearly evident.
Paper: A Disintegrating Rocky World Shrouded in Dust and Gas: Mid-infrared Observations of K2-22 b Using JWST
Authors: Nick Tusay, Jason T. Wright, Thomas G. Beatty, Steve Desch, Knicole Colón, Tushar Mittal, Hugh P. Osborn, Beatriz Campos Estrada, James E. Owen, Jessica Libby-Roberts, Arvind F. Gupta, Brad Foley, Erik Meier Valdés, Daniel J. Stevens, Ashley Herbst
Figure caption: Detrended CHEOPS photometry during transit 4. The red line is a second-order polynomial fit to the transit window and zero elsewhere. Multiple transit models were fit, including the original K2 lightcurve, a skewed Gaussian, and a boxcar, with no significant difference. The 46 minute transit duration calculated by R. Sanchis-Ojeda et al. (2015) is included for reference. Gaps in the data were caused by occultations of Earth during the space telescope’s orbit. The other three transit windows fall in these gaps.
Paper: Asymmetries in Fe IX 17.1 nm and Fe XII 19.5 nm Line Profiles as Possible Signatures of Obscuration Dimming in Sun-as-a-star Spectra
Authors: Yi-Bing Chen, Hong-Peng Lu, Hui Tian, He-Chao Chen, Ying Li, Zi-Hao Yang, Zheng Sun, Zhen-Yong Hou
Figure caption: Analysis of red–blue wing asymmetry in Fe IX 17.1 nm and Fe XII 19.5 nm lines during coronal dimming events. The figure presents two coronal dimming events associated with the eruptive flares of M9.3 class on 2013 October 24 (left column) and X5.4 class on 2012 March 7 (right column), with flare classifications indicated for each event. Panels (A) and (B) show the irradiance variations of Fe IX 17.1 nm and Fe XII 19.5 nm lines relative to the reference spectrum. Panels (C) and (D) display the red-wing and blue-wing irradiance variations of the Fe IX 17.1 nm line. Panels (E) and (F) illustrate the red-wing and blue-wing irradiance variations of the Fe XII 19.5 nm line. For both the Fe IX 17.1 nm and Fe XII 19.5 nm lines, the integration ranges for the red and blue wings are defined as the wavelength intervals corresponding to Doppler velocities of 0 to +1000 km s−1 and 0 to −1000 km s−1, respectively, relative to their rest wavelengths.
Paper: Polarized Multiwavelength Emission from Pulsar Wind—Accretion Disk Interaction in a Transitional Millisecond Pulsar
Authors: Maria Cristina Baglio, Francesco Coti Zelati, Alessandro Di Marco, Fabio La Monaca, Alessandro Papitto, Andrew K. Hughes, Sergio Campana, David M. Russell, Diego F. Torres, Francesco Carotenuto, Stefano Covino, Domitilla de Martino, Stefano Giarratana, Sara E. Motta, Kevin Alabarta, Paolo D'Avanzo, Giulia Illiano, Marco M. Messa, Arianna Miraval Zanon, Nanda Rea
Figure caption: Rotational (left) and orbital (right) phase dependence of the 2–6 keV normalized flux and polarization properties of J1023 in the high mode. From top to bottom, the left panel shows the pulse profile normalized to the average background-subtracted count rate as well as the normalized Stokes parameters qX and uX, the PX,H, and the PAX,H sampled in 10 phase bins as a function of the rotational phase and after background subtraction. From top to bottom, the right panel shows the normalized Stokes parameters qX and uX, the PX,H, and the PAX,H sampled in 10 phase bins as a function of the orbital phase and after background subtraction (here, phase 0 corresponds to the time of passage of the pulsar through the ascending node of the orbit). In both panels, upper limits are indicated with arrows and are reported at the 90% c.l. for bins compatible with null values at the 68% c.l. The PAX,H values are unconstrained for bins where upper limits on the PX,H have been derived. The red dashed line in the top-left panel indicates the best-fitting model comprising the fundamental and first harmonic components of the spin signal, whereas the red horizontal dashed lines in all other panels indicate the mean of the plotted polarization parameters. qX and uX are statistically consistent with remaining constant across the phases (see the text for more details).
Paper: Polarized Multiwavelength Emission from Pulsar Wind—Accretion Disk Interaction in a Transitional Millisecond Pulsar
Authors: Maria Cristina Baglio, Francesco Coti Zelati, Alessandro Di Marco, Fabio La Monaca, Alessandro Papitto, Andrew K. Hughes, Sergio Campana, David M. Russell, Diego F. Torres, Francesco Carotenuto, Stefano Covino, Domitilla de Martino, Stefano Giarratana, Sara E. Motta, Kevin Alabarta, Paolo D'Avanzo, Giulia Illiano, Marco M. Messa, Arianna Miraval Zanon, Nanda Rea
Figure caption: Top panels: IXPE time series extracted from the source region and binned at a 100 s resolution (black) and from the background region and binned at 1 ks (orange). Both time series were extracted by combining data from the three detector units, with the background time series rescaled to account for the area differences between the source and background extraction regions. The gaps in the time series correspond to time intervals when J1023 was obscured by the Earth. The vertical gray stripes mark the six time intervals of the simultaneous NICER observations, while the blue shaded area represents the time interval covered by VLT and VLA observations in the optical and radio bands. Bottom panels: IXPE and NICER time series for each overlapping time interval, with the NICER data binned at 10 s. The horizontal red dashed lines in the middle panels indicate the count-rate threshold adopted to differentiate between high and low mode episodes in the IXPE data set, while the cyan dashed lines in the bottom panels depict the NICER background level estimated using the SCORPEON model. The final part of the fifth time segment of the NICER data set is characterized by enhanced background level. Therefore, caution should be exercised in interpreting the corresponding increase in the count rate. BMJD stands for Barycentric Modified Julian Date, and TDB for Barycentric Dynamical Time.
Paper: Polarized Multiwavelength Emission from Pulsar Wind—Accretion Disk Interaction in a Transitional Millisecond Pulsar
Authors: Maria Cristina Baglio, Francesco Coti Zelati, Alessandro Di Marco, Fabio La Monaca, Alessandro Papitto, Andrew K. Hughes, Sergio Campana, David M. Russell, Diego F. Torres, Francesco Carotenuto, Stefano Covino, Domitilla de Martino, Stefano Giarratana, Sara E. Motta, Kevin Alabarta, Paolo D'Avanzo, Giulia Illiano, Marco M. Messa, Arianna Miraval Zanon, Nanda Rea
Figure caption: Geometry of polarized emission in the high mode of J1023. Pulsed emission originates from synchrotron emission at the boundary region where the pulsar particle wind—modulated at the NS rotational period—collides with the inner accretion flow at a distance of kRLC (k ≃ 1–2; RLC is the light cylinder radius; A. Papitto et al. 2019; A. Veledina et al. 2019). The magnetic field at the boundary region comprises both toroidal and poloidal components, with the constant X-ray PA across the pulsar phase indicating that the poloidal component is likely dominant. Particles in the region visible to the observer (orange filled circle) emit synchrotron radiation boosted perpendicular to the surface of the boundary region (orange shaded area). Black and red wave-like arrows represent X-ray and optical photons emitted from the boundary region. The average PA is defined as the angle between the north–south direction on the sky plane (cyan parallelogram) and the projected electric field vector (﹩\hat{{\bf{e}}}﹩). Gray double-ended arrows represent the amplitude of the electric field (not to scale). μ and Ω denote the pulsar magnetic moment and angular velocity vector, respectively.
Paper: Polarized Multiwavelength Emission from Pulsar Wind—Accretion Disk Interaction in a Transitional Millisecond Pulsar
Authors: Maria Cristina Baglio, Francesco Coti Zelati, Alessandro Di Marco, Fabio La Monaca, Alessandro Papitto, Andrew K. Hughes, Sergio Campana, David M. Russell, Diego F. Torres, Francesco Carotenuto, Stefano Covino, Domitilla de Martino, Stefano Giarratana, Sara E. Motta, Kevin Alabarta, Paolo D'Avanzo, Giulia Illiano, Marco M. Messa, Arianna Miraval Zanon, Nanda Rea
Figure caption: Variance distribution for the coherent pulsations of J1023 detected by IXPE. The distribution is derived from an epoch folding search of IXPE data filtered for the high mode in the 2–6 keV energy range. The folding variance is plotted against the frequency deviation from the IXPE-measured spin frequency, νIXPE = 592.42146705(9) Hz, marked with a vertical dashed line. The red solid curve indicates the best-fitting Gaussian function to the pulse variance distribution. The shaded areas indicate the uncertainty regions around the spin frequency measured by IXPE (gray) or those predicted by extrapolating the solutions reported by A. Burtovoi et al. (2020, B20; purple) and A. Jaodand et al. (2016, J16; green) to the epoch of the IXPE observation.
Paper: Polarized Multiwavelength Emission from Pulsar Wind—Accretion Disk Interaction in a Transitional Millisecond Pulsar
Authors: Maria Cristina Baglio, Francesco Coti Zelati, Alessandro Di Marco, Fabio La Monaca, Alessandro Papitto, Andrew K. Hughes, Sergio Campana, David M. Russell, Diego F. Torres, Francesco Carotenuto, Stefano Covino, Domitilla de Martino, Stefano Giarratana, Sara E. Motta, Kevin Alabarta, Paolo D'Avanzo, Giulia Illiano, Marco M. Messa, Arianna Miraval Zanon, Nanda Rea
Figure caption: Probability density function (pdf) of IXPE count rates and its modeling. The gray filled bins represent the distribution of count rates extracted from time series binned at 100 s. The gaps between some of the bins in the distribution result from the limited number of photon counts detected by IXPE in each time bin. The distribution was fit with a combination of three Gaussian functions. The blue line represents the pdf of the composite model that best fits the observed data. The brown curve represents the pdf of the Gaussian component associated with the high mode. The mean (μ) and standard deviation (σ), along with their 1σ uncertainties, are provided in the legend. The vertical red dashed line marks the threshold adopted to identify the flaring mode, set at 0.2 counts s−1, which corresponds to 4σ above the mean of the high mode component. The vertical axis is plotted on a logarithmic scale to highlight the tail of the distribution at higher count rates in the flaring mode.
Paper: Polarized Multiwavelength Emission from Pulsar Wind—Accretion Disk Interaction in a Transitional Millisecond Pulsar
Authors: Maria Cristina Baglio, Francesco Coti Zelati, Alessandro Di Marco, Fabio La Monaca, Alessandro Papitto, Andrew K. Hughes, Sergio Campana, David M. Russell, Diego F. Torres, Francesco Carotenuto, Stefano Covino, Domitilla de Martino, Stefano Giarratana, Sara E. Motta, Kevin Alabarta, Paolo D'Avanzo, Giulia Illiano, Marco M. Messa, Arianna Miraval Zanon, Nanda Rea
Figure caption: Evolution of the radio properties. The panels, from top to bottom, illustrate the temporal evolution of the radio flux density at the central frequency of 6 GHz in the VLA’s C band; the spectral index, calculated by dividing the 4–8 GHz band into two sub-bands (4–6 GHz and 6–8 GHz); and the 3σ upper limits on the linear polarization fraction. Each time bin represents a 2 minute interval. Spectral indices are only shown when they are constrained, with the horizontal dotted line marking a spectral index of 0 (i.e., a flat spectrum). BMJD stands for Barycentric Modified Julian Date, and TDB for Barycentric Dynamical Time.
Paper: Polarized Multiwavelength Emission from Pulsar Wind—Accretion Disk Interaction in a Transitional Millisecond Pulsar
Authors: Maria Cristina Baglio, Francesco Coti Zelati, Alessandro Di Marco, Fabio La Monaca, Alessandro Papitto, Andrew K. Hughes, Sergio Campana, David M. Russell, Diego F. Torres, Francesco Carotenuto, Stefano Covino, Domitilla de Martino, Stefano Giarratana, Sara E. Motta, Kevin Alabarta, Paolo D'Avanzo, Giulia Illiano, Marco M. Messa, Arianna Miraval Zanon, Nanda Rea
Figure caption: Normalized, background-subtracted Stokes parameters in the high mode in the 2–6 keV energy in distinct pulsar rotational phase bins. The results are derived from an unbinned analysis of the combined data from all three DUs. Each diamond represents the mean value for a phase bin, with the center of each phase bin highlighted in bordeaux. The corresponding shaded circular area shows the 1σ standard deviation. The circles give the contours of constant polarization degree while the radial lines correspond to constant polarization angle. Both diamonds and square areas are color-coded based on the normalized background-subtracted count rate in the corresponding pulse profile phase bin.
Paper: Polarized Multiwavelength Emission from Pulsar Wind—Accretion Disk Interaction in a Transitional Millisecond Pulsar
Authors: Maria Cristina Baglio, Francesco Coti Zelati, Alessandro Di Marco, Fabio La Monaca, Alessandro Papitto, Andrew K. Hughes, Sergio Campana, David M. Russell, Diego F. Torres, Francesco Carotenuto, Stefano Covino, Domitilla de Martino, Stefano Giarratana, Sara E. Motta, Kevin Alabarta, Paolo D'Avanzo, Giulia Illiano, Marco M. Messa, Arianna Miraval Zanon, Nanda Rea
Figure caption: SEDs for the high mode of J1023 derived from IXPE and VLT high-mode fluxes (green and red diamonds), with polarized fluxes depicted as squares. High-mode fluxes and pulsed fluxes in the X-ray and optical bands derived by A. Papitto et al. (2019) are shown as light-gray diamonds and circles, respectively. The gray dashed line represents the power-law fit to the pulsed fluxes.