adsabs/AstroCLIMB huggingface dataset:
Paper: SDSS-IV MaStar: Data-driven Parameter Derivation for the MaStar Stellar Library
Authors: Julie Imig, Jon A. Holtzman, Renbin Yan, Daniel Lazarz, Yanping Chen, Lewis Hill, Daniel Thomas, Claudia Maraston, Moire K. M. Prescott, Guy S. Stringfellow, Dmitry Bizyaev, Rachael L. Beaton, Niv Drory
Figure caption: Example fits for four randomly drawn spectra in different temperature bins from coolest (top row) to hottest (bottom row). For each star, its spectrum is shown on the left, with the observed spectrum (f obs)in black and the best-fit neural network model spectrum (f  nn ) in blue. The residuals for the spectral fit (f  nn  − f obs) are shown in the panel underneath the spectrum. The derived parameters are shown in a Kiel diagram on the right.
Paper: SDSS-IV MaStar: Data-driven Parameter Derivation for the MaStar Stellar Library
Authors: Julie Imig, Jon A. Holtzman, Renbin Yan, Daniel Lazarz, Yanping Chen, Lewis Hill, Daniel Thomas, Claudia Maraston, Moire K. M. Prescott, Guy S. Stringfellow, Dmitry Bizyaev, Rachael L. Beaton, Niv Drory
Figure caption: Parameters for the MaStar Stellar Library, presented in a Kiel diagram colored by [Fe/H] (left) and the [α/Fe]–[Fe/H] plane colored by effective temperature (right).
Paper: SDSS-IV MaStar: Data-driven Parameter Derivation for the MaStar Stellar Library
Authors: Julie Imig, Jon A. Holtzman, Renbin Yan, Daniel Lazarz, Yanping Chen, Lewis Hill, Daniel Thomas, Claudia Maraston, Moire K. M. Prescott, Guy S. Stringfellow, Dmitry Bizyaev, Rachael L. Beaton, Niv Drory
Figure caption: Parameters for the MaStar Stellar Library, plotted as a Kiel diagram colored by metallicity. Stellar isochrones from Bressan et al. (2012) are overplotted for reference, with a variety of stellar ages (dotted, dashed, or straight lines) and different metalicities (–2.5–0.5 in steps of 0.5, with the same color scale).
Paper: SDSS-IV MaStar: Data-driven Parameter Derivation for the MaStar Stellar Library
Authors: Julie Imig, Jon A. Holtzman, Renbin Yan, Daniel Lazarz, Yanping Chen, Lewis Hill, Daniel Thomas, Claudia Maraston, Moire K. M. Prescott, Guy S. Stringfellow, Dmitry Bizyaev, Rachael L. Beaton, Niv Drory
Figure caption: Resolution as a function of wavelength for each of the resolution-homogenzied MaStar catalogs released; the 99.5% resolution catalog (red), the 90% resolution catalog (yellow), the 75% resolution catalog (green), and the 60% resolution catalog (blue). The instrumental broadening value is a Gaussian σ in units of angstroms.
Paper: SDSS-IV MaStar: Data-driven Parameter Derivation for the MaStar Stellar Library
Authors: Julie Imig, Jon A. Holtzman, Renbin Yan, Daniel Lazarz, Yanping Chen, Lewis Hill, Daniel Thomas, Claudia Maraston, Moire K. M. Prescott, Guy S. Stringfellow, Dmitry Bizyaev, Rachael L. Beaton, Niv Drory
Figure caption: Left: parameters for the MaStar Stellar library shown in a Kiel diagram, colored by the reduced χ 2 value of our fits. Right: histogram showing the distribution of reduced χ 2 values.
Paper: HD 83443c: A Highly Eccentric Giant Planet on a 22 yr Orbit
Authors: Adriana Errico, Robert A. Wittenmyer, Jonathan Horner, Zhexing Li, G. Mirek Brandt, Stephen R. Kane, Tara Fetherolf, Timothy R. Holt, Brad Carter, Jake T. Clark, R. P. Butler, C. G. Tinney, Sarah Ballard, Brendan P. Bowler, John Kielkopf, Huigen Liu, Peter P. Plavchan, Avi Shporer, Hui Zhang, Duncan J. Wright, Brett C. Addison, Matthew W. Mengel, Jack Okumura
Figure caption: The mass of HD 83443c is the product of a lower limit set by radial velocities and a tight, astrometric upper limit constrained by its lack of acceleration between Hipparcos and Gaia eDR3. In red is the mass posterior from fitting radial velocities alone (i.e., the Gaussian m sin i constraint convolved with the sin i degeneracy). The black dashed line is the mass posterior implied by the lack of astrometric acceleration. The solid black line is the product of the red radial velocity posterior and the dashed-black astrometric posterior. The gray histogram is the resulting mass posterior from a joint orbital fit to the astrometry and radial velocities using orvara. The derived mass for HD 83443c is ﹩{1.5}_{-0.2}^{+0.5}{M}_{\mathrm{Jup}}﹩ with 1σ confidence and ﹩{1.5}_{-0.3}^{+2.0}{M}_{\mathrm{Jup}}﹩ with 3σ confidence.
Paper: HD 83443c: A Highly Eccentric Giant Planet on a 22 yr Orbit
Authors: Adriana Errico, Robert A. Wittenmyer, Jonathan Horner, Zhexing Li, G. Mirek Brandt, Stephen R. Kane, Tara Fetherolf, Timothy R. Holt, Brad Carter, Jake T. Clark, R. P. Butler, C. G. Tinney, Sarah Ballard, Brendan P. Bowler, John Kielkopf, Huigen Liu, Peter P. Plavchan, Avi Shporer, Hui Zhang, Duncan J. Wright, Brett C. Addison, Matthew W. Mengel, Jack Okumura
Figure caption:  RVSearch results for detectability of additional planets in the HD 83443 system. HD 83443b and c are shown as large black points, and the injected test planets are shown as small blue points. The solid black line indicates a 50% detection probability. HD 83443c lies within the region of high detectability, and the radial velocity data can exclude additional planets larger than ∼10–40  M ⊕ interior to 1 au, the region shown to be dynamically stable. The optimistic habitable zone is shaded in green.
Paper: HD 83443c: A Highly Eccentric Giant Planet on a 22 yr Orbit
Authors: Adriana Errico, Robert A. Wittenmyer, Jonathan Horner, Zhexing Li, G. Mirek Brandt, Stephen R. Kane, Tara Fetherolf, Timothy R. Holt, Brad Carter, Jake T. Clark, R. P. Butler, C. G. Tinney, Sarah Ballard, Brendan P. Bowler, John Kielkopf, Huigen Liu, Peter P. Plavchan, Avi Shporer, Hui Zhang, Duncan J. Wright, Brett C. Addison, Matthew W. Mengel, Jack Okumura
Figure caption: The observational data for HD 83443, color coded as follows: light blue, AAT (Tinney et al. 2001); green, HIRES/Keck (Tal-Or et al. 2019); blue, HARPS pre-correction (Trifonov et al. 2020); red, HARPS post correction (Trifonov et al. 2020); orange, MINERVA-Australis ThAr (Addison et al. 2019); and purple, MINERVA-Australis iodine (Addison et al. 2019). The top panel shows all the data as a function of time, with the two-planet solution shown in black. The center panel shows the data phase folded for HD 83443b only (center panel), with the lower panel showing the data for the long-period planet, HD 83443c (lower panel).
Paper: A Coronagraph with a Sub-λ/D Inner Working Angle and a Moderate Spectral Bandwidth
Authors: Satoshi Itoh, Taro Matsuo
Figure caption: Simulation of the core throughput and averaged leak (defined in Section 3.1) for different wavelengths. The red curves represent the averaged leak (the right vertical axes). The different-colored curves in each panel represent the core throughput for different separation angles of off-axis sources from a host star (the left vertical axes): 0.8–1.2λ 0/D (left), 0.3–0.7λ 0/D (center) and 1.3–1.7λ 0/D (right). The main reason for the decline in the core throughput for separation angles greater than 1.5λ 0/D is because the main peak of the PSF is no longer located at 1.0λ 0/D but 2.0λ 0/D.
Paper: A Coronagraph with a Sub-λ/D Inner Working Angle and a Moderate Spectral Bandwidth
Authors: Satoshi Itoh, Taro Matsuo
Figure caption: The final output PSFs of input monochromatic point sources at separation angles of 0.8λ 0/D (left), 1.0λ 0/D (center) and 1.2λ 0/D (right) for two observation wavelengths 675 (top), and 725 nm (bottom). Here, the x and y coordinates are normalized by λ 0/D, regardless of the observation wavelength. The peak locations of the PSFs shown here are approximately independent of both the angular separation and the observation wavelength.
Paper: A Coronagraph with a Sub-λ/D Inner Working Angle and a Moderate Spectral Bandwidth
Authors: Satoshi Itoh, Taro Matsuo
Figure caption: The optical layout for the performance simulation. The black and orange lines represent the light paths of on- and off-axis point sources, respectively. The abbreviations shown here have the following definitions: the first focal plane (F1), the first focal-plane mask (M1), the first pupil plane (P1), the first Lyot stop (L1), the second focal plane (F2), the second focal-plane mask (M2), the second pupil plane (P2), the second Lyot stop (L2), and the third (final) focal plane (F3).
Paper: A Coronagraph with a Sub-λ/D Inner Working Angle and a Moderate Spectral Bandwidth
Authors: Satoshi Itoh, Taro Matsuo
Figure caption: Left column: the normalized intensities of light observed on the focal and pupil planes coming from a point source on the optical axis. Center column: the normalized intensities of light from a point source at the separation angles of 1.0λ 0/D from the optical axis. Right column: the mask and Lyot-stop functions used in the performance simulation. The abbreviations shown here are the same as in Figure 1. The peak intensity at F1 is used to normalize all the intensities.
Paper: A Coronagraph with a Sub-λ/D Inner Working Angle and a Moderate Spectral Bandwidth
Authors: Satoshi Itoh, Taro Matsuo
Figure caption: Schematic for the region where we can achieve a core throughput higher than 10% and a contrast of 10−10 (blue filled areas). This schematic reflects the results of the simulation shown in Figure 4. Each region has a width of about 0.7λ 0/D. To save the telescope time, we need to know the target’s orbit by other observational methods to a precision higher than 0.7λ 0/D before observation.
Paper: Mapping out the Stellar Populations of IC 2602 and IC 2391
Authors: Azmain H. Nisak, Russel J. White, Alexandra Yep, Todd J. Henry, Leonardo Paredes, Hodari-Sadiki James, Wei-Chun Jao
Figure caption: For all 451 members of IC 2602 (top panels) and all 350 members of IC 2391 (bottom panels), histograms of parallax (left panels), proper motion in R.A. (center panels), and proper motion in decl. (right panels) are shown. Ensemble values for the distributions of these properties are listed in Table 2.
Paper: Mapping out the Stellar Populations of IC 2602 and IC 2391
Authors: Azmain H. Nisak, Russel J. White, Alexandra Yep, Todd J. Henry, Leonardo Paredes, Hodari-Sadiki James, Wei-Chun Jao
Figure caption: Histograms of radial velocity (left panels) and metallicity (right panels) for IC 2602 (top panels) and IC 2391 (bottom panels) are shown. Binaries are excluded as described in Section 6. Ensemble values for the distributions of these properties are listed in Table 2.
Paper: A Coronagraph with a Sub-λ/D Inner Working Angle and a Moderate Spectral Bandwidth
Authors: Satoshi Itoh, Taro Matsuo
Figure caption: The orthonormal base functions b  jk (α, β) that we used to expand low-order wave-front errors (j, k, ≤ 3).
Paper: HD 83443c: A Highly Eccentric Giant Planet on a 22 yr Orbit
Authors: Adriana Errico, Robert A. Wittenmyer, Jonathan Horner, Zhexing Li, G. Mirek Brandt, Stephen R. Kane, Tara Fetherolf, Timothy R. Holt, Brad Carter, Jake T. Clark, R. P. Butler, C. G. Tinney, Sarah Ballard, Brendan P. Bowler, John Kielkopf, Huigen Liu, Peter P. Plavchan, Avi Shporer, Hui Zhang, Duncan J. Wright, Brett C. Addison, Matthew W. Mengel, Jack Okumura
Figure caption: The amount of stirring experienced by the stable test particles that survived the full duration of our simulations of the HD 83443 system. Each individual dot plotted represents a test particle that survived until the end of our simulations. The top panels show, for each test particle, the difference between that particle’s initial and final semimajor axes (i.e., Δa = ∣a init − a final∣), while the lower panels show the change, for each test particle, in orbital eccentricity (i.e., Δe = ∣e init − e final). The left panels show the full range of semimajor axes considered in this work, while the right panel zooms in on the inner 0.75 au of the system, to show in more detail the fine structure in that region. The solid blue line connects all a − e locations with apocentre at the pericentre of the orbit of HD 83443c, with the dashed and dotted blue lines marking orbits with apocentres one and three Hill radii interior to HD 83443c’s pericenter. Similarly, the solid red line connects all orbits with apocenter or pericenter at the orbit of HD 83443b, such that all objects within the wedge described by the solid red line move on orbits that cross that of that planet. The red dashed and red dotted lines show orbits with pericenter three and five Hill radii beyond the orbit of HD 83443b, respectively. While orbits in the potential Habitable Zone around HD 83443 are stable (in that test particles in that region can survive the duration of the simulations), it is apparent that those particles experience significant stirring, primarily from HD 83443c, which would, at the very least, result in an planets in that region experiencing dramatic Milankovitch cycles, and may indicate that such orbits would prove unstable on longer timescales.
Paper: Globally Optimal and Scalable N-way Matching of Astronomy Catalogs
Authors: Tu Nguyen, Amitabh Basu, Tamás Budavári
Figure caption: An illustration of CanILP. As can be seen on the left side, we assume that there are two detections from Catalog 1 (Sources (1,1) and (2,1)), one detection from Catalog 2 (Source (1,2)), and two detections from Catalog 3 (Sources (1,3) and (2,3)). In CanILP, we list all candidates for possible associations across independent detections, which are shown on the right side. These are the x  T  in the formulation. We then find the combinations of subsets that maximize the overall likelihood. Here the solution given by CanILP indicates that the subsets {(1, 1), (2, 3)} and {(1, 2), (1, 3)} are included in the partition. These subsets, which are represented by a green color, correspond to the variables x {(1,1),(2,3)} = x {(1,2),(1,3)} = 1 in the model. On the other hand, all other variables x  T  = 0. Notice that Source (2,1) does not appear in any of these subsets, so we treat it as an orphan. As a result, the association outputted by CanILP is {{(1, 1), (2, 3)}, {(1, 2), (1, 3)}, {(2, 1)}}.
Paper: Globally Optimal and Scalable N-way Matching of Astronomy Catalogs
Authors: Tu Nguyen, Amitabh Basu, Tamás Budavári
Figure caption: Total running time comparison between the two formulations for the special case (log scale). Notice that CanILP chokes when there are 20 catalogs.
Paper: Globally Optimal and Scalable N-way Matching of Astronomy Catalogs
Authors: Tu Nguyen, Amitabh Basu, Tamás Budavári
Figure caption: An illustration of DirILP. As in Figure 1, assume that there are two detections from Catalog 1 (Sources (1,1) and (2,1)), one detection from Catalog 2 (Source (1,2)), and two detections from Catalog 3 (Sources (1,3) and (2,3)). In this case, the output of DirILP indicates that Sources (1,1) and (2,3) belong to the same object, that Sources (1,2) and (1,3) belong to the same object, and that Source (2,1) is an orphan. Notice that it is okay for an object to not have any source associated with it. The solution given by DirILP is {{(1, 1), (2, 3)}, {(1, 2), (1, 3)}, {(2, 1)}}, which is the same as the one given by CanILP in Figure 1.
Paper: Globally Optimal and Scalable N-way Matching of Astronomy Catalogs
Authors: Tu Nguyen, Amitabh Basu, Tamás Budavári
Figure caption: Total running time comparison between the two formulations for the general case (log scale). Notice that CanILP chokes when there are 18 catalogs.
Paper: Globally Optimal and Scalable N-way Matching of Astronomy Catalogs
Authors: Tu Nguyen, Amitabh Basu, Tamás Budavári
Figure caption: Optimization time comparison between the two formulations for the special case (log scale).
Paper: Globally Optimal and Scalable N-way Matching of Astronomy Catalogs
Authors: Tu Nguyen, Amitabh Basu, Tamás Budavári
Figure caption: Setup time comparison between the two formulations for the special case (log scale).
Paper: Globally Optimal and Scalable N-way Matching of Astronomy Catalogs
Authors: Tu Nguyen, Amitabh Basu, Tamás Budavári
Figure caption: Optimization time comparison between the two formulations for the general case (log scale).
Paper: Globally Optimal and Scalable N-way Matching of Astronomy Catalogs
Authors: Tu Nguyen, Amitabh Basu, Tamás Budavári
Figure caption: Total running time comparison between the two formulations when there are two detections from each catalog in an island (log scale).
Paper: Globally Optimal and Scalable N-way Matching of Astronomy Catalogs
Authors: Tu Nguyen, Amitabh Basu, Tamás Budavári
Figure caption: Setup time comparison between the two formulations for the general case (log scale).
Paper: TOI-1696: A Nearby M4 Dwarf with a 3 R ⊕ Planet in the Neptunian Desert
Authors: Mayuko Mori, John H. Livingston, Jerome de Leon, Norio Narita, Teruyuki Hirano, Akihiko Fukui, Karen A. Collins, Naho Fujita, Yasunori Hori, Hiroyuki Tako Ishikawa, Kiyoe Kawauchi, Keivan G. Stassun, Noriharu Watanabe, Steven Giacalone, Rebecca Gore, Ashley Schroeder, Courtney D. Dressing, Allyson Bieryla, Eric L. N. Jensen, Bob Massey, Avi Shporer, Masayuki Kuzuhara, David Charbonneau, David R. Ciardi, John P. Doty, Emma Esparza-Borges, Hiroki Harakawa, Klaus Hodapp, Masahiro Ikoma, Kai Ikuta, Keisuke Isogai, Jon M. Jenkins, Taiki Kagetani, Tadahiro Kimura, Takanori Kodama, Takayuki Kotani, Vigneshwaran Krishnamurthy, Tomoyuki Kudo, Seiya Kurita, Takashi Kurokawa, Nobuhiko Kusakabe, David W. Latham, Brian McLean, Felipe Murgas, Jun Nishikawa, Taku Nishiumi, Masashi Omiya, Hugh P. Osborn, Enric Palle, Hannu Parviainen, George R. Ricker, Sara Seager, Takuma Serizawa, Huan-Yu Teng, Yuka Terada, Joseph D. Twicken, Akitoshi Ueda, Roland Vanderspek, Sébastien Vievard, Joshua N. Winn, Yujie Zou, Motohide Tamura
Figure caption: Upper panels show the TESS PDCSAP light curve with the Savitzky–Golay (window = 1001) variability model (top), and the flattened light curve with the TLS model (bottom). The lower panels show the TLS power spectrum (left), folded TESS light curve with the TLS model (middle), and individual transit depths from the TLS (right).
Paper: TOI-1696: A Nearby M4 Dwarf with a 3 R ⊕ Planet in the Neptunian Desert
Authors: Mayuko Mori, John H. Livingston, Jerome de Leon, Norio Narita, Teruyuki Hirano, Akihiko Fukui, Karen A. Collins, Naho Fujita, Yasunori Hori, Hiroyuki Tako Ishikawa, Kiyoe Kawauchi, Keivan G. Stassun, Noriharu Watanabe, Steven Giacalone, Rebecca Gore, Ashley Schroeder, Courtney D. Dressing, Allyson Bieryla, Eric L. N. Jensen, Bob Massey, Avi Shporer, Masayuki Kuzuhara, David Charbonneau, David R. Ciardi, John P. Doty, Emma Esparza-Borges, Hiroki Harakawa, Klaus Hodapp, Masahiro Ikoma, Kai Ikuta, Keisuke Isogai, Jon M. Jenkins, Taiki Kagetani, Tadahiro Kimura, Takanori Kodama, Takayuki Kotani, Vigneshwaran Krishnamurthy, Tomoyuki Kudo, Seiya Kurita, Takashi Kurokawa, Nobuhiko Kusakabe, David W. Latham, Brian McLean, Felipe Murgas, Jun Nishikawa, Taku Nishiumi, Masashi Omiya, Hugh P. Osborn, Enric Palle, Hannu Parviainen, George R. Ricker, Sara Seager, Takuma Serizawa, Huan-Yu Teng, Yuka Terada, Joseph D. Twicken, Akitoshi Ueda, Roland Vanderspek, Sébastien Vievard, Joshua N. Winn, Yujie Zou, Motohide Tamura
Figure caption: Archival imaging from POSSII-F survey (taken in 1998; Reid et al. 1991) with the TESS photometric aperture (black outline) and Gaia sources (gray circles). The cyan circle indicates the position of TOI-1696; we note the proper motion is low enough that its current position is not significantly offset in the archival image.
Paper: TOI-1696: A Nearby M4 Dwarf with a 3 R ⊕ Planet in the Neptunian Desert
Authors: Mayuko Mori, John H. Livingston, Jerome de Leon, Norio Narita, Teruyuki Hirano, Akihiko Fukui, Karen A. Collins, Naho Fujita, Yasunori Hori, Hiroyuki Tako Ishikawa, Kiyoe Kawauchi, Keivan G. Stassun, Noriharu Watanabe, Steven Giacalone, Rebecca Gore, Ashley Schroeder, Courtney D. Dressing, Allyson Bieryla, Eric L. N. Jensen, Bob Massey, Avi Shporer, Masayuki Kuzuhara, David Charbonneau, David R. Ciardi, John P. Doty, Emma Esparza-Borges, Hiroki Harakawa, Klaus Hodapp, Masahiro Ikoma, Kai Ikuta, Keisuke Isogai, Jon M. Jenkins, Taiki Kagetani, Tadahiro Kimura, Takanori Kodama, Takayuki Kotani, Vigneshwaran Krishnamurthy, Tomoyuki Kudo, Seiya Kurita, Takashi Kurokawa, Nobuhiko Kusakabe, David W. Latham, Brian McLean, Felipe Murgas, Jun Nishikawa, Taku Nishiumi, Masashi Omiya, Hugh P. Osborn, Enric Palle, Hannu Parviainen, George R. Ricker, Sara Seager, Takuma Serizawa, Huan-Yu Teng, Yuka Terada, Joseph D. Twicken, Akitoshi Ueda, Roland Vanderspek, Sébastien Vievard, Joshua N. Winn, Yujie Zou, Motohide Tamura
Figure caption: Gemini/’Alopeke reconstructed images and contrast curves produced as described in Section 2.6.
Paper: TOI-1696: A Nearby M4 Dwarf with a 3 R ⊕ Planet in the Neptunian Desert
Authors: Mayuko Mori, John H. Livingston, Jerome de Leon, Norio Narita, Teruyuki Hirano, Akihiko Fukui, Karen A. Collins, Naho Fujita, Yasunori Hori, Hiroyuki Tako Ishikawa, Kiyoe Kawauchi, Keivan G. Stassun, Noriharu Watanabe, Steven Giacalone, Rebecca Gore, Ashley Schroeder, Courtney D. Dressing, Allyson Bieryla, Eric L. N. Jensen, Bob Massey, Avi Shporer, Masayuki Kuzuhara, David Charbonneau, David R. Ciardi, John P. Doty, Emma Esparza-Borges, Hiroki Harakawa, Klaus Hodapp, Masahiro Ikoma, Kai Ikuta, Keisuke Isogai, Jon M. Jenkins, Taiki Kagetani, Tadahiro Kimura, Takanori Kodama, Takayuki Kotani, Vigneshwaran Krishnamurthy, Tomoyuki Kudo, Seiya Kurita, Takashi Kurokawa, Nobuhiko Kusakabe, David W. Latham, Brian McLean, Felipe Murgas, Jun Nishikawa, Taku Nishiumi, Masashi Omiya, Hugh P. Osborn, Enric Palle, Hannu Parviainen, George R. Ricker, Sara Seager, Takuma Serizawa, Huan-Yu Teng, Yuka Terada, Joseph D. Twicken, Akitoshi Ueda, Roland Vanderspek, Sébastien Vievard, Joshua N. Winn, Yujie Zou, Motohide Tamura
Figure caption: Palomar/PHARO images and contrast curves (top: Brγ; bottom: Hcont) produced as described in Section 2.7.
Paper: HD 83443c: A Highly Eccentric Giant Planet on a 22 yr Orbit
Authors: Adriana Errico, Robert A. Wittenmyer, Jonathan Horner, Zhexing Li, G. Mirek Brandt, Stephen R. Kane, Tara Fetherolf, Timothy R. Holt, Brad Carter, Jake T. Clark, R. P. Butler, C. G. Tinney, Sarah Ballard, Brendan P. Bowler, John Kielkopf, Huigen Liu, Peter P. Plavchan, Avi Shporer, Hui Zhang, Duncan J. Wright, Brett C. Addison, Matthew W. Mengel, Jack Okumura
Figure caption: The dynamical stability of massless test particles in the HD 83443 system, as a function of their initial semimajor axis and eccentricity, from simulations spanning a period of 1 Myr. The stability of the inner region of the system is dominated by the influence of HD 83443b, with test particles that approach that planet too closely being removed from the system on short timescales. In the outer regions of the system, stability is strongly influenced by HD 83443c, which renders most orbits beyond ∼1.5 au unstable due to its high eccentricity (reaching a periastron distance of 1.92 au). We note that, since the simulations covered a period of 1 Myr, the regions in white are those where test particles have minimum lifetimes of 1 Myr. It is highly likely that, across much of that space, lifetimes would be far longer than the 1 Myr of our simulations.