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<jats:title>Abstract</jats:title> <jats:p>We reassess the <jats:sup>65</jats:sup>As(p,<jats:italic>γ</jats:italic>)<jats:sup>66</jats:sup>Se reaction rates based on a set of proton thresholds of <jats:sup>66</jats:sup>Se, <jats:italic>S</jats:italic> <jats:sub>p</jats:sub>(<jats:sup>66</jats:sup>Se), estimated from the experimental mirror nuclear masses, theoretical mirror displacement energies, and full <jats:italic>p</jats:italic> <jats:italic>f</jats:italic>-model space shell-model calculation. The self-consistent relativistic Hartree–Bogoliubov theory is employed to obtain the mirror displacement energies with much reduced uncertainty, and thus reducing the proton-threshold uncertainty up to 161 keV compared to the AME2020 evaluation. Using the simulation instantiated by the one-dimensional multi-zone hydrodynamic code, K<jats:sc>epler</jats:sc>, which closely reproduces the observed GS 1826−24 clocked bursts, the present forward and reverse <jats:sup>65</jats:sup>As(p,<jats:italic>γ</jats:italic>)<jats:sup>66</jats:sup>Se reaction rates based on a selected <jats:italic>S</jats:italic> <jats:sub>p</jats:sub>(<jats:sup>66</jats:sup>Se) = 2.469 ± 0.054 MeV, and the latest <jats:sup>22</jats:sup>Mg(<jats:italic>α</jats:italic>,p)<jats:sup>25</jats:sup>Al, <jats:sup>56</jats:sup>Ni(p,<jats:italic>γ</jats:italic>)<jats:sup>57</jats:sup>Cu, <jats:sup>57</jats:sup>Cu(p,<jats:italic>γ</jats:italic>)<jats:sup>58</jats:sup>Zn, <jats:sup>55</jats:sup>Ni(p,<jats:italic>γ</jats:italic>)<jats:sup>56</jats:sup>Cu, and <jats:sup>64</jats:sup>Ge(p,<jats:italic>γ</jats:italic>)<jats:sup>65</jats:sup>As reaction rates, we find that though the GeAs cycles are weakly established in the rapid-proton capture process path, the <jats:sup>65</jats:sup>As(p,<jats:italic>γ</jats:italic>)<jats:sup>66</jats:sup>Se reaction still strongly characterizes the burst tail end due to the two-proton sequential capture on <jats:sup>64</jats:sup>Ge, not found by the Cyburt et al. sensitivity study. The <jats:sup>65</jats:sup>As(p,<jats:italic>γ</jats:italic>)<jats:sup>66</jats:sup>Se reaction influences the abundances of nuclei <jats:italic>A</jats:italic> = 64, 68, 72, 76, and 80 up to a factor of 1.4. The new <jats:italic>S</jats:italic> <jats:sub>p</jats:sub>(<jats:sup>66</jats:sup>Se) and the inclusion of the updated <jats:sup>22</jats:sup>Mg(<jats:italic>α</jats:italic>,p)<jats:sup>25</jats:sup>Al reaction rate increases the production of <jats:sup>12</jats:sup>C up to a factor of 4.5, which is not observable and could be the main fuel for a superburst. The enhancement of the <jats:sup>12</jats:sup>C mass fraction alleviates the discrepancy in explaining the origin of the superburst. The waiting point status of and two-proton sequential capture on <jats:sup>64</jats:sup>Ge, the weak-cycle feature of GeAs at a region heavier than <jats:sup>64</jats:sup>Ge, and the impact of other possible <jats:italic>S</jats:italic> <jats:sub>p</jats:sub>(<jats:sup>66</jats:sup>Se) are also discussed.</jats:p>

<jats:title>Abstract</jats:title> <jats:p>During the X-ray bursts of GS 1826−24, a “clocked burster”, the nuclear reaction flow that surges through the rapid-proton capture process path has to pass through the NiCu cycles before reaching the ZnGa cycles that moderate further hydrogen burning in the region above the germanium and selenium isotopes. The <jats:sup>57</jats:sup>Cu(p,<jats:italic>γ</jats:italic>)<jats:sup>58</jats:sup>Zn reaction that occurs in the NiCu cycles plays an important role in influencing the burst light curves found by Cyburt et al. We deduce the <jats:sup>57</jats:sup>Cu(p,<jats:italic>γ</jats:italic>)<jats:sup>58</jats:sup>Zn reaction rate based on the experimentally determined important nuclear structure information, isobaric-multiplet-mass equation, and large-scale shell-model calculations. Based on the isobaric-multiplet-mass equation, we propose a possible order of <jats:inline-formula> <jats:tex-math> <?CDATA ${1}_{1}^{+}$?> </jats:tex-math> <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:msubsup> <mml:mrow> <mml:mn>1</mml:mn> </mml:mrow> <mml:mrow> <mml:mn>1</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>+</mml:mo> </mml:mrow> </mml:msubsup> </mml:math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjac4d89ieqn1.gif" xlink:type="simple" /> </jats:inline-formula>- and <jats:inline-formula> <jats:tex-math> <?CDATA ${2}_{3}^{+}$?> </jats:tex-math> <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:msubsup> <mml:mrow> <mml:mn>2</mml:mn> </mml:mrow> <mml:mrow> <mml:mn>3</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>+</mml:mo> </mml:mrow> </mml:msubsup> </mml:math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjac4d89ieqn2.gif" xlink:type="simple" /> </jats:inline-formula>-dominant resonance states and constrain the resonance energy of the <jats:inline-formula> <jats:tex-math> <?CDATA ${1}_{2}^{+}$?> </jats:tex-math> <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:msubsup> <mml:mrow> <mml:mn>1</mml:mn> </mml:mrow> <mml:mrow> <mml:mn>2</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>+</mml:mo> </mml:mrow> </mml:msubsup> </mml:math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjac4d89ieqn3.gif" xlink:type="simple" /> </jats:inline-formula> state. The latter reduces the contribution of the <jats:inline-formula> <jats:tex-math> <?CDATA ${1}_{2}^{+}$?> </jats:tex-math> <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:msubsup> <mml:mrow> <mml:mn>1</mml:mn> </mml:mrow> <mml:mrow> <mml:mn>2</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>+</mml:mo> </mml:mrow> </mml:msubsup> </mml:math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjac4d89ieqn4.gif" xlink:type="simple" /> </jats:inline-formula>-dominant resonance state. The new reaction rate is up to a factor of 4 lower than the Forstner et al. rate recommended by JINA REACLIB v2.2 at the temperature regime sensitive to clocked bursts of GS 1826−24. Using the simulation from the one-dimensional implicit hydrodynamic code K<jats:sc>epler</jats:sc> to model the thermonuclear X-ray bursts of the GS 1826−24 clocked burster, we find that the new <jats:sup>57</jats:sup>Cu(p,<jats:italic>γ</jats:italic>)<jats:sup>58</jats:sup>Zn reaction rate, coupled with the latest <jats:sup>56</jats:sup>Ni(p,<jats:italic>γ</jats:italic>)<jats:sup>57</jats:sup>Cu and <jats:sup>55</jats:sup>Ni(p,<jats:italic>γ</jats:italic>)<jats:sup>56</jats:sup>Cu reaction rates, redistributes the reaction flow in the NiCu cycles and strongly influences the burst ash composition, whereas the <jats:sup>59</jats:sup>Cu(p,<jats:italic>α</jats:italic>)<jats:sup>56</jats:sup>Ni and <jats:sup>59</jats:sup>Cu(p,<jats:italic>γ</jats:italic>)<jats:sup>60</jats:sup>Zn reactions suppress the influence of the <jats:sup>57</jats:sup>Cu(p,<jats:italic>γ</jats:italic>)<jats:sup>58</jats:sup>Zn reaction and diminish the impact of nuclear reaction flow that bypasses the important <jats:sup>56</jats:sup>Ni waiting point induced by the <jats:sup>55</jats:sup>Ni(p,<jats:italic>γ</jats:italic>)<jats:sup>56</jats:sup>Cu reaction on the burst light curve.</jats:p>

<jats:title>Abstract</jats:title> <jats:p>We present a survey of the central region of the nearest starburst galaxy, IC 10, using the W. M. Keck Observatory Keck Cosmic Web Imager (KCWI) at high spectral and spatial resolution. We map the central starburst of IC 10 to sample the kinematic and ionization properties of the individual star-forming regions. Using the low spectral resolution mode of KCWI, we map the oxygen abundance, and with the high spectral resolution mode, we identify 46 individual H <jats:sc>II</jats:sc> regions. These H <jats:sc>II</jats:sc> regions have an average radius of 4.0 pc, star formation rate ∼1.3 × 10<jats:sup>−4</jats:sup> <jats:italic>M</jats:italic> <jats:sub>⊙</jats:sub> yr<jats:sup>−1</jats:sup>, and velocity dispersion ∼16 km s<jats:sup>−1</jats:sup>. None of the H <jats:sc>II</jats:sc> regions appear to be virialized (<jats:italic>α</jats:italic> <jats:sub>vir</jats:sub> ≫ 1), and on average, they show evidence of ongoing expansion. IC 10's H <jats:sc>II</jats:sc> regions are offset from the star-forming-region size–luminosity scaling relationships, as well as Larson’s Law that relates size and velocity dispersion. We investigate the balance of inward and outward pressure, <jats:italic>P</jats:italic> <jats:sub>in</jats:sub> and <jats:italic>P</jats:italic> <jats:sub>out</jats:sub>, finding <jats:italic>P</jats:italic> <jats:sub>out</jats:sub> &gt; <jats:italic>P</jats:italic> <jats:sub>in</jats:sub> in 89% of H <jats:sc>II</jats:sc> regions, indicating feedback-driven expansion even in these low-mass H <jats:sc>II</jats:sc> regions. We find warm gas pressure (<jats:italic>P</jats:italic> <jats:sub>gas</jats:sub>) provides the dominant contribution to the outward pressure (<jats:italic>P</jats:italic> <jats:sub>out</jats:sub>). This counteracts the inward pressure, which is dominated by turbulence in the surrounding gas rather than self-gravity. Five H <jats:sc>II</jats:sc> regions show evidence of outflows that are most likely supported by either stellar winds (two regions) or champagne flows (three regions). These observations provide new insights into the state of the star-forming regions in IC 10 and negative feedback from low-mass clusters.</jats:p>

<jats:title>Abstract</jats:title> <jats:p>The physical properties responsible for the formation and evolution of the corona and heliosphere are still not completely understood. 3D MHD global modeling is a powerful tool to investigate all the possible candidate processes. To fully understand the role of each of them, we need a validation process where the output from the simulations is quantitatively compared to the observational data. In this work, we present the results from our validation process applied to the wave turbulence driven 3D MHD corona-wind model WindPredict-AW. At this stage of the model development, we focus the work to the coronal regime in quiescent condition. We analyze three simulation results, which differ by the boundary values. We use the 3D distributions of density and temperature, output from the simulations at the time of around the first Parker Solar Probe perihelion (during minimum of the solar activity), to synthesize both extreme ultraviolet (EUV) and white-light-polarized (WL pB) images to reproduce the observed solar corona. For these tests, we selected AIA 193 Å, 211 Å, and 171 Å EUV emissions, MLSO K-Cor, and LASCO C2 pB images obtained on 2018 November 6 and 7. We then make quantitative comparisons of the disk and off limb corona. We show that our model is able to produce synthetic images comparable to those of the observed corona.</jats:p>

<jats:title>Abstract</jats:title> <jats:p>We present Markov Chain Monte Carlo radiative transfer modeling of a joint ALMA 345 GHz and spectral energy distribution data set for a sample of 97 protostellar disks from the VLA and ALMA Nascent Disk and Multiplicity Survey of Orion Protostars. From this modeling, we derive disk and envelope properties for each protostar, allowing us to examine the bulk properties of a population of young protostars. We find that disks are small, with a median dust radius of <jats:inline-formula> <jats:tex-math> <?CDATA ${29.4}_{-2.7}^{+4.1}$?> </jats:tex-math> <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:msubsup> <mml:mrow> <mml:mn>29.4</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>−</mml:mo> <mml:mn>2.7</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>+</mml:mo> <mml:mn>4.1</mml:mn> </mml:mrow> </mml:msubsup> </mml:math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjac574dieqn1.gif" xlink:type="simple" /> </jats:inline-formula> au and a median dust mass of <jats:inline-formula> <jats:tex-math> <?CDATA ${5.8}_{-2.7}^{+4.6}$?> </jats:tex-math> <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:msubsup> <mml:mrow> <mml:mn>5.8</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>−</mml:mo> <mml:mn>2.7</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>+</mml:mo> <mml:mn>4.6</mml:mn> </mml:mrow> </mml:msubsup> </mml:math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjac574dieqn2.gif" xlink:type="simple" /> </jats:inline-formula> <jats:italic>M</jats:italic> <jats:sub>⊕</jats:sub>. We find no statistically significant difference between most properties of Class 0, Class I, and flat-spectrum sources with the exception of envelope dust mass and inclination. The distinction between inclination is an indication that the Class 0/I/flat-spectrum system may be difficult to tie uniquely to the evolutionary state of protostars. When comparing with Class II disk dust masses in Taurus from similar radiative transfer modeling, we further find that the trend of disk dust mass decreasing from Class 0 to Class II disks is no longer present, though it remains unclear whether such a comparison is fair owing to differences in star-forming region and modeling techniques. Moreover, the disks we model are broadly gravitationally stable. Finally, we compare disk masses and radii with simulations of disk formation and find that magnetohydrodynamical effects may be important for reproducing the observed properties of disks.</jats:p>

<jats:title>Abstract</jats:title> <jats:p>We use a geometric method to derive (two-dimensional) separation functions among pairs of objects within populations of specified position function <jats:inline-formula> <jats:tex-math> <?CDATA ${dN}/d{\boldsymbol{R}}$?> </jats:tex-math> <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:mi mathvariant="italic">dN</mml:mi> <mml:mrow> <mml:mo stretchy="true">/</mml:mo> </mml:mrow> <mml:mi>d</mml:mi> <mml:mi mathvariant="bold-italic">R</mml:mi> </mml:math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjac5b5fieqn1.gif" xlink:type="simple" /> </jats:inline-formula>. We present analytic solutions for separation functions corresponding to a uniform surface density within a circular field, a Plummer sphere (viewed in projection), and the mixture thereof—including contributions from binary objects within both subpopulations. These results enable inferences about binary object populations via direct modeling of object position and pair separation data, without resorting to standard estimators of the two-point correlation function. Analyzing mock data sets designed to mimic known dwarf spheroidal galaxies, we demonstrate the ability to recover input properties including the number of wide binary star systems and, in cases where the number of resolved binary pairs is assumed to be ≳a few hundred, characteristic features (e.g., steepening and/or truncation) of their separation function. Combined with forthcoming observational capabilities, this methodology opens a window onto the formation and/or survival of wide binary populations in dwarf galaxies, and offers a novel probe of inferred dark matter substructure on the smallest galactic scales.</jats:p>

<jats:title>Abstract</jats:title> <jats:p>We present ultraviolet spectroscopy covering the Ly<jats:italic>α</jats:italic> + N <jats:sc>v</jats:sc> complex of six candidate low-redshift (0.9 &lt; <jats:italic>z</jats:italic> &lt; 1.5) weak emission-line quasars (WLQs) based on observations with the Hubble Space Telescope. The original systematic searches for these puzzling Type 1 quasars with intrinsically weak broad emission lines revealed an <jats:italic>N</jats:italic> ≈ 100 WLQ population from optical spectroscopy of high-redshift (<jats:italic>z</jats:italic> &gt; 3) quasars, defined by a Ly<jats:italic>α</jats:italic> + N <jats:sc>v</jats:sc> rest-frame equivalent width (EW) threshold &lt;15.4 Å. Identification of lower-redshift (<jats:italic>z</jats:italic> &lt; 3) WLQ candidates, however, has relied primarily on optical spectroscopy of weak broad emission lines at longer rest-frame wavelengths. With these new observations expanding existing optical coverage into the ultraviolet, we explore unifying the low- and high-<jats:italic>z</jats:italic> WLQ populations via EW[Ly<jats:italic>α</jats:italic>+N <jats:sc>v</jats:sc>]. Two objects in the sample unify with high-<jats:italic>z</jats:italic> WLQs, three others appear consistent with the intermediate portion of the population connecting WLQs and normal quasars, and the final object is consistent with typical quasars. The expanded wavelength coverage improves the number of available line diagnostics for our individual targets, allowing a better understanding of the shapes of their ionizing continua. The ratio of EW[Ly<jats:italic>α</jats:italic>+N <jats:sc>v</jats:sc>] to EW[Mg <jats:sc>ii</jats:sc>] in our sample is generally small but varied, favoring a soft ionizing continuum scenario for WLQs, and we find a lack of correlation between EW[Ly<jats:italic>α</jats:italic>+N <jats:sc>v</jats:sc>] and the X-ray properties of our targets, consistent with a “slim-disk” shielding gas model. We also find indications that weak absorption may be a more significant contaminant in low-<jats:italic>z</jats:italic> WLQ populations than previously thought.</jats:p>

<jats:title>Abstract</jats:title> <jats:p>We present a <jats:italic>z</jats:italic> = 0.94 quasar, SDSS J004846.45-004611.9, discovered in the Sloan Digital Sky Survey III (SDSS-III) BOSS survey. A visual analysis of this spectrum reveals highly broadened and blueshifted narrow emission lines, in particular, [Ne <jats:sc>v</jats:sc>] <jats:italic>λ</jats:italic>3426 and [O <jats:sc>iii</jats:sc>] <jats:italic>λ</jats:italic>5007, with outflow velocities of 4000 km s<jats:sup>−1</jats:sup>, along with unusually large [Ne <jats:sc>v</jats:sc>] <jats:italic>λ</jats:italic>3426/[Ne <jats:sc>iii</jats:sc>] <jats:italic>λ</jats:italic>3869 ratios. The gas shows higher ionization at higher outflow velocities, indicating a connection between the powerful outflow and the unusual strength of the high ionization lines. The spectral energy distribution and the <jats:italic>i</jats:italic> − W3 color of the source reveal that it is likely a <jats:italic>core</jats:italic> extremely red quasar (ERQ); a candidate population of young active galactic nuclei (AGN) that are violently <jats:italic>blowing out</jats:italic> gas and dust from their centers. The dominance of host galaxy light in its spectrum and its fortuitous position in the SDSS S82 region allows us to measure its star formation history and investigate variability for the first time in an ERQ. Our analysis indicates that SDSS J004846.45-004611.9 underwent a short-lived starburst phase 400 Myr ago and was subsequently quenched, possibly indicating a time lag between star formation quenching and the onset of AGN activity. We also find that the strong extinction can be uniquely attributed to the AGN and does not persist in the host galaxy, contradicting a scenario where the source has recently transitioned from being a dusty submillimeter galaxy. In our relatively shallow photometric data, the source does not appear to be variable at 0.24–2.4 <jats:italic>μ</jats:italic>m in the rest frame, most likely due to the dominant contribution of host galaxy starlight at these wavelengths.</jats:p>

<jats:title>Abstract</jats:title> <jats:p>In the canonical theory of stellar magnetic dynamo, the tachocline in partially convective stars serves to arrange small-scale fields, generated by stochastic movement of plasma into a coherent large-scale field. Mid-to-late-type M dwarfs, which are fully convective, show more magnetic activity than classical magnetic dynamo theory predicts. However, mid-to-late-type M dwarfs show tight correlations between rotation and magnetic activity, consistent with elements of classical dynamo theory. We use data from the Magellan Inamori Kyocera Echelle Spectrograph to detail the relation between Ca <jats:sc>ii</jats:sc> H and K flux and rotation period for these low-mass stars. We measure <jats:inline-formula> <jats:tex-math> <?CDATA ${R}_{\mathrm{HK}}^{{\prime} }$?> </jats:tex-math> <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:msubsup> <mml:mrow> <mml:mi>R</mml:mi> </mml:mrow> <mml:mrow> <mml:mi>HK</mml:mi> </mml:mrow> <mml:mrow> <mml:mo accent="true">′</mml:mo> </mml:mrow> </mml:msubsup> </mml:math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjac5cbfieqn1.gif" xlink:type="simple" /> </jats:inline-formula> values for 53 spectroscopically identified M dwarfs selected from the MEarth survey; these stars span spectral classes from M5.0 to M3.5 and have rotation periods ranging from hours to months. We present the rotation–activity relationship as traced through these data. We find power-law and saturated regimes consistent to within 1<jats:italic>σ</jats:italic> of previously published results and observe a mass dependence in <jats:inline-formula> <jats:tex-math> <?CDATA ${R}_{\mathrm{HK}}^{{\prime} }$?> </jats:tex-math> <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:msubsup> <mml:mrow> <mml:mi>R</mml:mi> </mml:mrow> <mml:mrow> <mml:mi>HK</mml:mi> </mml:mrow> <mml:mrow> <mml:mo accent="true">′</mml:mo> </mml:mrow> </mml:msubsup> </mml:math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjac5cbfieqn2.gif" xlink:type="simple" /> </jats:inline-formula>.</jats:p>

<jats:title>Abstract</jats:title> <jats:p>We present a detailed analysis of the rest-frame UV and optical emission-line spectrum of the partially obscured quasar J121704.70+023417.1 (hereafter J1217+0234). Here the obscuring material, very likely the dusty torus invoked by the AGN unification models, acts as a natural coronagraph, which greatly suppresses both the continuum and broad-line emission in the UV and enables a clear detection of three emission-line components at and beyond the dusty torus scale: (1) The component, with a blueshift of <jats:italic>v</jats:italic> ≈ 1200 km s<jats:sup>−1</jats:sup> and a line width of FWHM ≈ 2600 km s<jats:sup>−1</jats:sup>, shows exceptionally large intensity ratios, such as N <jats:sc>v</jats:sc>/Ly<jats:italic>α</jats:italic> ≈ 2.3 and O <jats:sc>vi</jats:sc>/Ly<jats:italic>α</jats:italic> ≈ 1.4, indicating that the emitting gas is highly ionized and has a very high density up to <jats:italic>n</jats:italic> <jats:sub>H</jats:sub> ∼ 10<jats:sup>13</jats:sup> cm<jats:sup>−3</jats:sup>, possibly associated with the dusty torus. (2) The largely unshifted narrow-line component, with FWHM ≈ 510 km s<jats:sup>−1</jats:sup>, is completely absent in all UV lines but Ly<jats:italic>α </jats:italic>and is significantly detected in the forbidden lines of [O <jats:sc>iii</jats:sc>], [O <jats:sc>ii</jats:sc>], and [Ne <jats:sc>iii</jats:sc>] in the optical, implying massive low-density (<jats:italic>n</jats:italic> <jats:sub>H</jats:sub> ∼ 10<jats:sup>2</jats:sup> cm<jats:sup>−3</jats:sup>) gas ∼40 kpc from the galactic center. (3) The intermediate component is only detected in [O <jats:sc>iii</jats:sc>] with a blueshift and line width between (1) and (2), which might bridge the gases from the circumnuclear to the circumgalactic scales. Follow-up observations with high spatial resolution and high sensitivity are needed to confirm the speculation and are helpful to reveal outflows at multiscales in J1217+0234.</jats:p>