adsabs/AstroCLIMB huggingface dataset:
Paper: A Possible Mechanism for the “Late Phase” in Stellar White-light Flares
Authors: Kai E. Yang, 凯 杨, Xudong Sun, 旭东 孙, Graham S. Kerr, Hugh S. Hudson
Figure caption: (a) Illustration of our 1D loop model. The locations of the heating sources are colored in brown for the loop apex and footpoints as in Equation (2). (b) Normalized temporal profiles of the heating rate for the apex f t(t) (blue solid line) and footpoints f b(t) (dotted lines) for the three different cases listed in Table 1 (orange, green, red). The decay timescales of the footpoint heating rate are 14.5, 29.5, and 59.5 minutes, respectively. The left and right portions depict the initial impulsive loop-top heating and the late-time gradual footpoint heating processes, respectively. They are discontinuous and have different scales on the horizontal axis.
Paper: A Possible Mechanism for the “Late Phase” in Stellar White-light Flares
Authors: Kai E. Yang, 凯 杨, Xudong Sun, 旭东 孙, Graham S. Kerr, Hugh S. Hudson
Figure caption: Tracing a plasma parcel (initial position l = −13.65 Mm at time t = 8 minutes) in Case 1 by integrating its velocity over time. Top left: the trajectory of the parcel overlaid on the velocity stack plot. Top right: evolution of temperature. Bottom left: evolution number density. Bottom right: the corresponding relative TESS flux, and contribution from free–free, free-bound, and Thomson scattering mechanisms.
Paper: A Possible Mechanism for the “Late Phase” in Stellar White-light Flares
Authors: Kai E. Yang, 凯 杨, Xudong Sun, 旭东 孙, Graham S. Kerr, Hugh S. Hudson
Figure caption: Same as Figure 3, but for Cases 11–13 with asymmetric footpoint heat sources.
Paper: A Possible Mechanism for the “Late Phase” in Stellar White-light Flares
Authors: Kai E. Yang, 凯 杨, Xudong Sun, 旭东 孙, Graham S. Kerr, Hugh S. Hudson
Figure caption: Same as Figure 3, but for Cases 7 and 8 (R L = 10 Mm, with half and double footpoint source heating timescales, i.e., τ d,b = 14.5 and 59.5 minutes). They can be compared with Case 3 (τ d,b = 29.5 minutes) in Figure 3.
Paper: A Possible Mechanism for the “Late Phase” in Stellar White-light Flares
Authors: Kai E. Yang, 凯 杨, Xudong Sun, 旭东 孙, Graham S. Kerr, Hugh S. Hudson
Figure caption: The relative emission contribution along the loop and its evolution in time, which is evaluated from Equations (A1)–(A3). The area between the two red dashed lines indicates the corona portion.
Paper: A Possible Mechanism for the “Late Phase” in Stellar White-light Flares
Authors: Kai E. Yang, 凯 杨, Xudong Sun, 旭东 孙, Graham S. Kerr, Hugh S. Hudson
Figure caption: Same as Figure 3, but for Cases 4–6 (R L = 30 Mm).
Paper: A Possible Mechanism for the “Late Phase” in Stellar White-light Flares
Authors: Kai E. Yang, 凯 杨, Xudong Sun, 旭东 孙, Graham S. Kerr, Hugh S. Hudson
Figure caption: Same as Figure 3, but for Cases 9 and 10 (R L = 10 Mm) with only footpoint and loop-top heating sources, respectively. The white arrow points out the region with catastrophic cooling and no plasma condensation.
Paper: Observations of a Failed Solar Filament Eruption Involving External Reconnection
Authors: Yuehong Chen, 悦虹 陈, Xin Cheng, 鑫 程, Jun Chen, 俊 陈, Yu Dai, 煜 戴, Mingde Ding, 明德 丁
Figure caption: (a) Distance–time plot of the AIA 304 Å images along the slit in Figure 1(c2); the blue circles denote the height–time measurements of the leading front of the filament. (b) The GOES 1–8 Å SXR flux and the temporal evolution of the filament velocity, with the errors from the uncertainty in height measurements (∼2 pixels, 877 km). (c) The HXR flux of the Fermi 25–50 keV channel and the time derivative of the GOES SXR flux. A 10 s smoothing is applied to the latter. The blue and red backgrounds in panels (b) and (c) indicate the acceleration phase and deceleration phase, respectively.
Paper: Premerger Sky Localization of Gravitational Waves from Binary Neutron Star Mergers Using Deep Learning
Authors: Chayan Chatterjee, Linqing Wen
Figure caption: Architecture of our model, GW-SkyLocator. The input data, consisting of the S/N time series, ρ(t), and intrinsic parameters, θ in, are provided to the network through two separate channels: the ResNet-34 channel (only one ResNet block is shown here) and the multilayered fully connected (Dense) network, respectively. The features extracted by ρ(t) and θ in are then combined and provided as conditional input to the main component of GW-SkyLocator–the MAF network, denoted by f(z). The MAF draws samples, z, from a multivariate Gaussian and learns mapping between z to (α, δ), which are the R.A. and decl. angles of the GW events.
Paper: Observations of a Failed Solar Filament Eruption Involving External Reconnection
Authors: Yuehong Chen, 悦虹 陈, Xin Cheng, 鑫 程, Jun Chen, 俊 陈, Yu Dai, 煜 戴, Mingde Ding, 明德 丁
Figure caption: (a) The radial component of the Lambert cylindrical equal-area (CEA) vector magnetic field from SHARP with a linear scale saturating at 500 G; white (black) regions are positive (negative). The white arrows denote the inner and the outer polarities. (b), (c) The extrapolated 3D potential field structure from the side and top views; the center-lobe flux, side-lobe flux, and high-lying flux are in blue, green, and red, respectively. The gray ball indicates the position of the null point.
Paper: Premerger Sky Localization of Gravitational Waves from Binary Neutron Star Mergers Using Deep Learning
Authors: Chayan Chatterjee, Linqing Wen
Figure caption: (a)–(f): P–P plots for test samples at 0, 10, 15, 28, 44, and 58 s before the merger. The figure shows the cumulative distribution function of the searched probability, which should lie close to the diagonal (dashed line) if GW-SkyLocator's posterior distributions are accurate. The gray band shows the 95% confidence band.
Paper: Premerger Sky Localization of Gravitational Waves from Binary Neutron Star Mergers Using Deep Learning
Authors: Chayan Chatterjee, Linqing Wen
Figure caption: (a) Box and whiskers plots showing the areas of the 90% credible intervals from GW-SkyLocator (blue) and BAYESTAR (pink) at 0, 10, 15, 28, 44, and 58 s before the merger. The boxes encompass 95% of the events and the whiskers extend up to the rest. The white lines within the boxes represent the median values of the respective data sets. (b) Similar box and whiskers plot as in (a) for comparing searched areas from GW-SkyLocator (blue) and BAYESTAR (pink) at 0, 10, 15, 28, 44, and 58 s before the merger.
Paper: Premerger Sky Localization of Gravitational Waves from Binary Neutron Star Mergers Using Deep Learning
Authors: Chayan Chatterjee, Linqing Wen
Figure caption: Top panel from (a) to (c): histograms of the areas of the 90% credible intervals of 2000 BNS events obtained from GW-SkyLocator (blue) and BAYESTAR (orange) for 0, 10, and 15 s before the merger. Bottom panel from (d) to (f): similar histograms for 28, 44, and 58 s before the merger.
Paper: Premerger Sky Localization of Gravitational Waves from Binary Neutron Star Mergers Using Deep Learning
Authors: Chayan Chatterjee, Linqing Wen
Figure caption: Top panel from (a) to (c): histograms of the searched areas of 2000 BNS events obtained from GW-SkyLocator (blue) and BAYESTAR (orange) for 0, 10, and 15 s before the merger. Bottom panel from (d) to (f): similar histograms for 28, 44, and 58 s before the merger.
Paper: JWST NIRCam Observations of SN 1987A: Spitzer Comparison and Spectral Decomposition
Authors: Richard G. Arendt, Martha L. Boyer, Eli Dwek, Mikako Matsuura, Aravind P. Ravi, Armin Rest, Roger Chevalier, Phil Cigan, Ilse De Looze, Guido De Marchi, Claes Fransson, Christa Gall, R. D. Gehrz, Haley L. Gomez, Tuomas Kangas, Florian Kirchschlager, Robert P. Kirshner, Josefin Larsson, Peter Lundqvist, Dan Milisavljevic, Sangwook Park, Nathan Smith, Jason Spyromilio, Tea Temim, Lifan Wang, J. Craig Wheeler, Charles E. Woodward
Figure caption: NIRCam images of SN 1987A reprojected onto a common (α, δ) coordinate grid. The top row contains the broadband images. The middle row shows narrowband images that are respectively centered on lines for: [Fe II]+[Si I], H2, H2 (also), and H I. The images are logarithmically scaled from 0.32 to 32 MJy sr−1 (after adding an offset of 0.5 MJy sr−1) and show a field of view of 5″ × 5″. North is up and east is to the left in all images in this paper. The red dots in the lower left corner of each panel indicate the FWHM size of the PSF. The relative brightness variations between the inner ejecta, the hotspots of the ER, and the emission beyond the ER hotspots indicate a variety of emission mechanisms at work. The bottom row emphasizes the line emission in each of the narrow bands by subtracting scaled versions of the wideband emission.
Paper: JWST NIRCam Observations of SN 1987A: Spitzer Comparison and Spectral Decomposition
Authors: Richard G. Arendt, Martha L. Boyer, Eli Dwek, Mikako Matsuura, Aravind P. Ravi, Armin Rest, Roger Chevalier, Phil Cigan, Ilse De Looze, Guido De Marchi, Claes Fransson, Christa Gall, R. D. Gehrz, Haley L. Gomez, Tuomas Kangas, Florian Kirchschlager, Robert P. Kirshner, Josefin Larsson, Peter Lundqvist, Dan Milisavljevic, Sangwook Park, Nathan Smith, Jason Spyromilio, Tea Temim, Lifan Wang, J. Craig Wheeler, Charles E. Woodward
Figure caption: The top row shows (left) apertures used to replicate the IRAC photometry that had been performed on much lower-resolution data, and (right) the resulting SED. These flux densities are the sum of those for the SN and stars 2, 3, and 4. The horizontal lines indicate the bandwidths for wide bands (filled circles) and narrow bands (open circles). The middle row shows results with a smaller aperture that includes only the SN. Star 3 is specifically excluded from the background region. The bottom row shows the SEDs of stars 2, 3, and 4, with 21,000 K stellar atmosphere models from Coelho (2014) shown for comparison. Star 3 is a classical Be star with excess emission at >3 μm. The green dashed line shows the SED of the B2IIIe star SMC5_074402 from Bonanos et al. (2010) for comparison (multiplied by a factor of 0.8). The display range on the bottom left panel is altered such that the stars are not saturated.
Paper: JWST NIRCam Observations of SN 1987A: Spitzer Comparison and Spectral Decomposition
Authors: Richard G. Arendt, Martha L. Boyer, Eli Dwek, Mikako Matsuura, Aravind P. Ravi, Armin Rest, Roger Chevalier, Phil Cigan, Ilse De Looze, Guido De Marchi, Claes Fransson, Christa Gall, R. D. Gehrz, Haley L. Gomez, Tuomas Kangas, Florian Kirchschlager, Robert P. Kirshner, Josefin Larsson, Peter Lundqvist, Dan Milisavljevic, Sangwook Park, Nathan Smith, Jason Spyromilio, Tea Temim, Lifan Wang, J. Craig Wheeler, Charles E. Woodward
Figure caption: Correlation of the brightness in the inner ER (at F405N) and the outer ER (at F444W). Top: brightness as a function of deprojected position angle along the Figure 8 ellipses tracing the bright hotspots (blue) and the outer emission (red, multiplied by 5). Position angle is measured eastward from north along the ring as if it were viewed face on. The dotted lines show the large-scale variation as traced by the lowest-frequency components of the Fourier transform. Bottom: the small-scale structure of the bright hotspots (blue) and outer emission (red, multiplied by 5) after subtraction of the large-scale background indicated in the top panel. The spots in the outer portion of the ER are anticorrelated in position angle with the bright hotspots with a correlation coefficient of −0.38.
Paper: JWST NIRCam Observations of SN 1987A: Spitzer Comparison and Spectral Decomposition
Authors: Richard G. Arendt, Martha L. Boyer, Eli Dwek, Mikako Matsuura, Aravind P. Ravi, Armin Rest, Roger Chevalier, Phil Cigan, Ilse De Looze, Guido De Marchi, Claes Fransson, Christa Gall, R. D. Gehrz, Haley L. Gomez, Tuomas Kangas, Florian Kirchschlager, Robert P. Kirshner, Josefin Larsson, Peter Lundqvist, Dan Milisavljevic, Sangwook Park, Nathan Smith, Jason Spyromilio, Tea Temim, Lifan Wang, J. Craig Wheeler, Charles E. Woodward
Figure caption: The IRAC light curves at 3.6 and 4.5 μm are shown with filled circles. The NIRCam measurements are indicated with filled stars at day 12,975. Formal random uncertainties are smaller than the plotted symbols. For consistency with the IRAC measurements, these are the large-aperture flux densities minus 0.41 and 0.26 mJy estimates for the 3.6 and 4.5 μm combined brightness of Stars 2 and 3. The dashed red line shows that an extrapolation of the IRAC model (solid red line; Arendt et al. 2020) is a good predictor of the NIRCam flux densities. The IRAC models are the convolution of a Gaussian function and an exponential function (shown as black curves at d 0).
Paper: JWST NIRCam Observations of SN 1987A: Spitzer Comparison and Spectral Decomposition
Authors: Richard G. Arendt, Martha L. Boyer, Eli Dwek, Mikako Matsuura, Aravind P. Ravi, Armin Rest, Roger Chevalier, Phil Cigan, Ilse De Looze, Guido De Marchi, Claes Fransson, Christa Gall, R. D. Gehrz, Haley L. Gomez, Tuomas Kangas, Florian Kirchschlager, Robert P. Kirshner, Josefin Larsson, Peter Lundqvist, Dan Milisavljevic, Sangwook Park, Nathan Smith, Jason Spyromilio, Tea Temim, Lifan Wang, J. Craig Wheeler, Charles E. Woodward
Figure caption: Locations of ER hotspots and clumps. Left: images at F444W (red), F405N (green), and F200W (blue). Right: F444W image superimposed with ellipses tracing the bright hotspots (blue) and the outer emission (red) as shown in Figure 9.
Paper: JWST NIRCam Observations of SN 1987A: Spitzer Comparison and Spectral Decomposition
Authors: Richard G. Arendt, Martha L. Boyer, Eli Dwek, Mikako Matsuura, Aravind P. Ravi, Armin Rest, Roger Chevalier, Phil Cigan, Ilse De Looze, Guido De Marchi, Claes Fransson, Christa Gall, R. D. Gehrz, Haley L. Gomez, Tuomas Kangas, Florian Kirchschlager, Robert P. Kirshner, Josefin Larsson, Peter Lundqvist, Dan Milisavljevic, Sangwook Park, Nathan Smith, Jason Spyromilio, Tea Temim, Lifan Wang, J. Craig Wheeler, Charles E. Woodward
Figure caption: 3.6 μm stellar photometry (light curves) of stars 2, 3, and 4. The filled circles are modeled brightnesses from IRAC data (Arendt et al. 2020), where the stars are not fully resolved. The filled star symbols at day 12,975 indicate NIRCam measurements. Stars 2 and 4 appear to be stable, while Star 3 (a classical Be star) appears to show a decreased brightness. Star 3 is intrinsically variable, but, in addition, the IRAC flux densities may have been affected by confusion with the ER.
Paper: JWST NIRCam Observations of SN 1987A: Spitzer Comparison and Spectral Decomposition
Authors: Richard G. Arendt, Martha L. Boyer, Eli Dwek, Mikako Matsuura, Aravind P. Ravi, Armin Rest, Roger Chevalier, Phil Cigan, Ilse De Looze, Guido De Marchi, Claes Fransson, Christa Gall, R. D. Gehrz, Haley L. Gomez, Tuomas Kangas, Florian Kirchschlager, Robert P. Kirshner, Josefin Larsson, Peter Lundqvist, Dan Milisavljevic, Sangwook Park, Nathan Smith, Jason Spyromilio, Tea Temim, Lifan Wang, J. Craig Wheeler, Charles E. Woodward
Figure caption: Comparison of IRAC and NIRCam images at comparable wavelengths provides a qualitative indication that the high-resolution mapping and deconvolution of the IRAC data (Arendt et al. 2020) had revealed hints of the true structure of the SNR emission, and that there have been no major changes between the Spitzer and JWST eras.
Paper: Evidence for Low-power Radio Jet–ISM Interaction at 10 pc in the Dwarf AGN Host NGC 4395
Authors: Payel Nandi, C. S. Stalin, D. J. Saikia, Rogemar A. Riffel, Arijit Manna, Sabyasachi Pal, O. L. Dors, Dominika Wylezalek, Vaidehi S. Paliya, Payaswini Saikia, Pratik Dabhade, Markus-Kissler Patig, Ram Sagar
Figure caption: Left: the VLA radio images at 15 GHz with a size of 1″ × 1″. The contours are at 0.03, 0.05, and 0.10 mJy beam−1. The rms noise is 11 μJy beam−1. Here, C is the radio core, E is the eastern jet component and W is the western jet component. Right: the 4.8 GHz VLA image with a size of 5″ × 5″. The contours are at 0.15, 0.20, 0.40, 0.50, and 0.60 mJy beam−1. The rms noise is 48 μJy beam−1. The synthesized beams are shown as white ellipses. These have a size of 0.″129  ×  0.″124 with a PA of −18° (left panel) and 1.″75  ×  1.″19 with a PA of 89° (right panel). The red cross in both panels represents the optical Gaia position.
Paper: Evidence for Low-power Radio Jet–ISM Interaction at 10 pc in the Dwarf AGN Host NGC 4395
Authors: Payel Nandi, C. S. Stalin, D. J. Saikia, Rogemar A. Riffel, Arijit Manna, Sabyasachi Pal, O. L. Dors, Dominika Wylezalek, Vaidehi S. Paliya, Payaswini Saikia, Pratik Dabhade, Markus-Kissler Patig, Ram Sagar
Figure caption: The position of the spaxels belonging to the central 1″ ×  1″ region of NGC 4395 in the line-ratio diagnostic diagrams. The green solid curve is from Kauffmann et al. (2003), black and red solid lines are from Kewley et al. (2001). The typical error in these plots is 0.01 dex in both axes.
Paper: Evidence for Low-power Radio Jet–ISM Interaction at 10 pc in the Dwarf AGN Host NGC 4395
Authors: Payel Nandi, C. S. Stalin, D. J. Saikia, Rogemar A. Riffel, Arijit Manna, Sabyasachi Pal, O. L. Dors, Dominika Wylezalek, Vaidehi S. Paliya, Payaswini Saikia, Pratik Dabhade, Markus-Kissler Patig, Ram Sagar
Figure caption: GMOS [O III]λ5007 image in color scale along with the radio emission at 15 GHz (green contours) with contour levels of 0.03, 0.08, and 0.1 mJy beam−1 and HST [O III]λ5007 emission (black contours) with contour levels of (0.05, 0.1, 0.2, 1.0) × 10−15 erg s−1 cm−2. The left panel shows the GMOS total flux in [O III]λ5007, the middle panel shows the GMOS flux in the narrow component of [O III]λ5007 and the right-hand panel shows the GMOS flux in the broad component of [O III]λ5007. The red cross is the core (optical Gaia position). The green circle is the synthesized beam of 15 GHz data with a size of 0.″129  ×  0.″124 along PA −18°.
Paper: Evidence for Low-power Radio Jet–ISM Interaction at 10 pc in the Dwarf AGN Host NGC 4395
Authors: Payel Nandi, C. S. Stalin, D. J. Saikia, Rogemar A. Riffel, Arijit Manna, Sabyasachi Pal, O. L. Dors, Dominika Wylezalek, Vaidehi S. Paliya, Payaswini Saikia, Pratik Dabhade, Markus-Kissler Patig, Ram Sagar
Figure caption: Left panel: distribution of spaxels belonging to the 1″ × 1″ region of NGC 4395 in the asymmetry index vs. the velocity dispersion plane. Right panel: distribution of spaxels belonging to the 1″ × 1″ region in the W90 ([O III]λ5007 line) vs. the intensity ratio of the [N II]λ6584 and Hα lines.
Paper: Evidence for Low-power Radio Jet–ISM Interaction at 10 pc in the Dwarf AGN Host NGC 4395
Authors: Payel Nandi, C. S. Stalin, D. J. Saikia, Rogemar A. Riffel, Arijit Manna, Sabyasachi Pal, O. L. Dors, Dominika Wylezalek, Vaidehi S. Paliya, Payaswini Saikia, Pratik Dabhade, Markus-Kissler Patig, Ram Sagar
Figure caption: Comparison between predictions of the line ratios due to photoionization by AGN (left panel) and shocks (right panel) and the observed line ratios. The clustered black points are the observed data points in central 1″ ×  1″. The model grids are shown for different shock velocities, magnetic fields, and ionization parameters. The typical error of the data points in these plots is 0.01 dex in both axes.
Paper: Evidence for Low-power Radio Jet–ISM Interaction at 10 pc in the Dwarf AGN Host NGC 4395
Authors: Payel Nandi, C. S. Stalin, D. J. Saikia, Rogemar A. Riffel, Arijit Manna, Sabyasachi Pal, O. L. Dors, Dominika Wylezalek, Vaidehi S. Paliya, Payaswini Saikia, Pratik Dabhade, Markus-Kissler Patig, Ram Sagar
Figure caption: Upper panel: the continuum emission at 237 GHz based on observations with ALMA on 2018 March 22 (left) and 2019 January 23 (right). The contours are -0.08, 0.08, 0.09, and 0.1 Jy beam−1 (left) and −0.08, 0.08, 0.1, and 0.2 Jy beam−1 (right). Lower panel: the CO(2−1) emission for the observation on 2018 March 22 (left) and 2019 January 23 (right). The contours are 0.02, 0.04, 0.05, 0.06, and 0.07 Jy beam−1 km s−1 (left) and 0.05, 0.1, 0.2, 0.4, and 0.5 Jy beam−1 km s−1 (right). The red cross is the optical Gaia position. The synthesized beams are shown by black ellipses.
Paper: Evidence for Low-power Radio Jet–ISM Interaction at 10 pc in the Dwarf AGN Host NGC 4395
Authors: Payel Nandi, C. S. Stalin, D. J. Saikia, Rogemar A. Riffel, Arijit Manna, Sabyasachi Pal, O. L. Dors, Dominika Wylezalek, Vaidehi S. Paliya, Payaswini Saikia, Pratik Dabhade, Markus-Kissler Patig, Ram Sagar
Figure caption: Temperature plot. Here, the yellow point refers to NGC 4395. The blue curve is the AGN photoionization grid. The black and red points are from Dors et al. (2020) and Riffel et al. (2021), respectively.
Paper: Evidence for Low-power Radio Jet–ISM Interaction at 10 pc in the Dwarf AGN Host NGC 4395
Authors: Payel Nandi, C. S. Stalin, D. J. Saikia, Rogemar A. Riffel, Arijit Manna, Sabyasachi Pal, O. L. Dors, Dominika Wylezalek, Vaidehi S. Paliya, Payaswini Saikia, Pratik Dabhade, Markus-Kissler Patig, Ram Sagar
Figure caption: The rest-frame spectrum of NGC 4395 from MaNGA covering the central brightest 0.″5  ×  0.″5. The lines used to calculate the line intensity ratios are marked.
Paper: Evidence for Low-power Radio Jet–ISM Interaction at 10 pc in the Dwarf AGN Host NGC 4395
Authors: Payel Nandi, C. S. Stalin, D. J. Saikia, Rogemar A. Riffel, Arijit Manna, Sabyasachi Pal, O. L. Dors, Dominika Wylezalek, Vaidehi S. Paliya, Payaswini Saikia, Pratik Dabhade, Markus-Kissler Patig, Ram Sagar
Figure caption: Left panel: temperature map from [N II] line ratio. Right panel: temperature difference map with respect to the central spaxel. The red cross is the optical Gaia position.
Paper: Evidence for Low-power Radio Jet–ISM Interaction at 10 pc in the Dwarf AGN Host NGC 4395
Authors: Payel Nandi, C. S. Stalin, D. J. Saikia, Rogemar A. Riffel, Arijit Manna, Sabyasachi Pal, O. L. Dors, Dominika Wylezalek, Vaidehi S. Paliya, Payaswini Saikia, Pratik Dabhade, Markus-Kissler Patig, Ram Sagar
Figure caption: Plot of flux density against frequency. The solid lines are linear least squares fits to the data. The orange line is the fit to all the data points, while the green line is the fit excluding the 8.4 GHz measurement.
Paper: Evidence for Low-power Radio Jet–ISM Interaction at 10 pc in the Dwarf AGN Host NGC 4395
Authors: Payel Nandi, C. S. Stalin, D. J. Saikia, Rogemar A. Riffel, Arijit Manna, Sabyasachi Pal, O. L. Dors, Dominika Wylezalek, Vaidehi S. Paliya, Payaswini Saikia, Pratik Dabhade, Markus-Kissler Patig, Ram Sagar
Figure caption: Schematic diagram of our proposed scenario in the inner region of NGC 4395. The jet during its travels outward from the central radio core, interacts with the medium and ionizes the gas via shock excitation. The radio core coincides with the optical Gaia position, the peak of the [O III] emission, and the peak of the 237 GHz emission. Ionized [O III] has a cone-like structure, with the radio jet along the axis and causing the outflows. The CO(2−1) gas is located northward by ∼1″ from the radio core. While ionized [O III]λ5007, warm molecular H2λ2.4085 emissions are along the jet, there is a lack of cold CO in the vicinity, which is possibly due to interactions with the radio jet. As cold gas is needed for the SF process, the lack of cold gas naturally leads to conditions less favorable for SF at scales of ∼10 pc close to the center of NGC 4395.