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+<div id="title">
+
+# Spectral and magnetic properties of the jet base in NGC 315
+
+</div>
+<div id="comments">
+
+[![arXiv](https://img.shields.io/badge/arXiv-2411.19126-b31b1b.svg)](https://arxiv.org/abs/2411.19126)<mark>Appeared on: 2024-12-02</mark> -  _16 pages, 19 figures, accepted for publication in A&A_
+
+</div>
+<div id="authors">
+
+L. Ricci, et al. -- incl., <mark>G. Mattia</mark>
+
+</div>
+<div id="abstract">
+
+**Abstract:**            The dynamic of relativistic jets in the inner parsec regions is deeply affected by the nature of the magnetic fields. The level of magnetization of the plasma, as well as the geometry of these fields on compact scales, have not yet been fully constrained. In this paper we employ multi-frequency and multi-epoch very long baseline interferometry observations of the nearby radio galaxy NGC 315. We aim to derive insights into the magnetic field properties on sub-parsec and parsec scales by examining observational signatures such as the spectral index, synchrotron turnover frequency, and brightness temperature profiles. This analysis is performed by considering the properties of the jet acceleration and collimation zone, which can be probed thanks to the source vicinity, as well as the inner part of the jet conical region. We observe remarkably steep values for the spectral index on sub-parsec scales ($\alpha \sim -2$, $S_\nu \propto \nu^\alpha$) which flatten around $\alpha \sim -0.8$ on parsec scales. We suggest that the observed steep values may result from particles being accelerated via diffusive shock acceleration mechanisms in magnetized plasma and subsequently experiencing cooling through synchrotron losses. The brightness temperature of the 43 GHz cores indicates a dominance of the magnetic energy at the jet base, while the cores at progressively lower frequencies reveal a gradual transition towards equipartition. Based on the spectral index and brightness temperature along the incoming jet, and by employing theoretical models, we derive that the magnetic field strength has a close-to-linear dependence with distance going from parsec scales up to the jet apex. Overall, our findings are consistent with a toroidal-dominated magnetic field on all the analyzed scales.         
+
+</div>
+
+<div id="div_fig1">
+
+<img src="tmp_2411.19126/./Images/Core_shift_VLBA.png" alt="Fig2" width="100%"/>
+
+**Figure 2. -** Core position as a function of frequency for the two different data sets: i) the multi-frequency VLBA data set (orange points); ii) the multi-frequency and multi-epoch data set presented in [Boccardi, Perucho and Casadio (2021)]()(blue points). The blue line represents the best-fit values presented in [Boccardi, Perucho and Casadio (2021)](), the orange line traces the best-fit performed in this paper by employing all the data, and the purple line highlights the best-fit curve obtained using only the data points at 8, 15, 22, and 43 GHz. (*fig:core_shift*)
+
+</div>
+<div id="div_fig2">
+
+<img src="tmp_2411.19126/./Images/Turnover_frequency_profile.png" alt="Fig3" width="100%"/>
+
+**Figure 3. -** Turnover frequency along the ridgeline as a function of distance from the 43 GHz core. The multiple data points at the same distance are from the different possible core-shift configurations. The orange points represent the upper boundary, while the green ones the lower boundary. The turnover frequency decreases from $10   \mathrm{GHz} \lesssim \nu_\mathrm{br} \lesssim 35   \mathrm{GHz}$ in the 43 GHz core, down to $\sim 6   \mathrm{GHz}$ at $\sim 0.7   \mathrm{pc}$. (*fig:turnover_evolution*)
+
+</div>
+<div id="div_fig3">
+
+<img src="tmp_2411.19126/./Images/VLBA_SM_profiles_5_perc_3.png" alt="Fig7" width="100%"/>
+
+**Figure 7. -** Average spectral index as a function of distance from the 43 GHz core for different pairs of frequencies. In addition to the VLBA data set here presented, we re-present for comparison the 22-43 GHz spectral index values for the two epochs presented by [Ricci, Boccardi and Nokhrina (2022)](). At high frequencies, remarkably steep spectral index values down to $\alpha \sim -2$ are observed within one parsec from the core, corresponding to ${\sim}10^4   R_\mathrm{S}$. Downstream, a convergence towards flatter values $\alpha \sim -0.8$ is observed at all frequencies. The black vertical lines highlight the jet break point, as proposed in  ([Boccardi, Perucho and Casadio 2021]()) , while the horizontal dashed line is set at $\alpha = -1$ as reference. (*fig:alpha_profiles*)
+
+</div><div id="qrcode"><img src=https://api.qrserver.com/v1/create-qr-code/?size=100x100&data="https://arxiv.org/abs/2411.19126"></div>

docs/_build/html/2411.19489.md

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+<div id="title">
+
+# ATOMS: ALMA Three-millimeter Observations of Massive Star-forming regions – $\uppercase$$\expandafter{\romannumeral19}$. The origin of SiO emission
+
+</div>
+<div id="comments">
+
+[![arXiv](https://img.shields.io/badge/arXiv-2411.19489-b31b1b.svg)](https://arxiv.org/abs/2411.19489)<mark>Appeared on: 2024-12-02</mark> -  _23 pages, 14 figures_
+
+</div>
+<div id="authors">
+
+R. Liu, et al. -- incl., <mark>S. Li</mark>
+
+</div>
+<div id="abstract">
+
+**Abstract:** The production of silicon monoxide (SiO) can be considered as a fingerprint of shock interaction.In this work, we use high-sensitivity observations of the SiO (2-1) and H $^{13}$ CO $^{+}$ (1-0) emission to investigate the broad and narrow SiO emission toward 146 massive star-forming regions in the ATOMS survey. We detected SiO emission in 136 regions and distinguished broad and narrow components across the extension of 118 sources (including 58 UC H ii regions) with an average angular resolution of 2.5 $^{\prime}^{\prime}$ .The derived SiO luminosity ( $L_\textup{SiO}$ ) across the whole sample shows that the majority of $L_\textup{SiO}$ (above 66 $\%$ ) can be attributed to broad SiO, indicating its association with strong outflows.The comparison of the ALMA SiO images with the filamentary skeletons identified from H $^{13}$ CO $^{+}$ and in the infrared data (at 4.5, 8, and 24 $\upmu$ m), further confirms that most SiO emission originates from outflows. However, note that for nine sources in our sample, the observed SiO emission may be generated by expanding UC H ii regions. There is a moderate positive correlation between the bolometric luminosity ( $L_\textup{bol}$ ) and $L_\textup{SiO}$ for both components (narrow and broad). The UC H ii sources show a weaker positive correlation between $L_\textup{bol}$ and $L_\textup{SiO}$ and higher $L_\textup{SiO}$ compared to the sources without UC H ii regions. These results imply that the SiO emission from UC H ii sources might be affected by UV-photochemistry induced by UC H ii regions.
+
+</div>
+
+<div id="div_fig1">
+
+<img src="tmp_2411.19489/./Figure/Figure10/LM_Lsio_N_new_final.png" alt="Fig10" width="100%"/>
+
+**Figure 10. -** _ Upper panels_: The SiO luminosity ($L_\textup{sio}$) versus  bolometric luminosity ($L_\textup{bol}$).
+The filled and empty gray stars present broad and narrow SiO components in _A groups_ without UC Hii regions, and the filled and empty gray circles depict broad and narrow SiO
+components in _B groups_ without UC Hii regions.
+The filled and empty red stars show broad and narrow SiO components in _A groups_ hosting UC Hii regions, while the filled and empty red circles display broad and narrow SiO components in _B groups_ with UC Hii regions.
+The filled green rectangles show the low-mass stars  (2022MNRAS.512.5214D, [Jiménez-Serra, et. al 2011](https://ui.adsabs.harvard.edu/abs/2011ApJ...739...80J), [Spezzano, et. al 2020](https://ui.adsabs.harvard.edu/abs/2020A&A...640A..74S), [Santiago-García, et. al 2009](https://ui.adsabs.harvard.edu/abs/2009A&A...495..169S), [ and Lee 2020](https://ui.adsabs.harvard.edu/abs/2020A&ARv..28....1L)) .
+In the upper left panel, the gray line shows a linear fit of log $(L_\textrm{sio} / L_{\sun})$$= (0.64\pm0.07)$ log $(L_\textrm{bol} / L_{\sun})$ - $6.98\pm0.32$ obtained for sources without UC Hii regions, while the red line shows the linear fit log $(L_\textrm{sio} / L_{\sun})$$ = (0.56\pm0.11)$ log $(L_\textrm{bol} / L_{\sun})$ - $6.81\pm0.58$ obtained for sources hosting UC Hii sources.
+In the upper right panel, the gray line displays the linear fit
+log $(L_\textrm{sio} / L_{\sun})$$ = (0.65\pm0.08)$ log $(L_\textrm{bol} / L_{\sun})$ - $7.30\pm0.33$ derived for sources without UC Hii regions, while the red line is used to show the linear fit
+log $(L_\textrm{sio} / L_{\sun})$$ = (0.40\pm0.13)$ log $(L_\textrm{bol} / L_{\sun})$ - $6.31\pm0.68$ inferred for sources hosting UC Hii regions.
+_ Lower panels_: $L_\textup{sio}$ vs. $L_\textup{bol}/M$. No apparent correlation is seen either for the broad or for the narrow components. The symbols are the same as in the upper panels. (*fig10*)
+
+</div>
+<div id="div_fig2">
+
+<img src="tmp_2411.19489/./Figure/Figure3/I08470-4243.moment04.png" alt="Fig4.1" width="25%"/><img src="tmp_2411.19489/./Figure/Figure3/I11332-6258.moment010.png" alt="Fig4.2" width="25%"/><img src="tmp_2411.19489/./Figure/Figure3/I11298-6155.moment09.png" alt="Fig4.3" width="25%"/><img src="tmp_2411.19489/./Figure/Figure3/I12326-6245.moment013.png" alt="Fig4.4" width="25%"/>
+
+**Figure 4. -** Four representative sources imaged with ALMA within the ATOMS program. The background corresponds to the SiO (2-1) integrated intensity maps. The black contours show the 3 mm continuum emission detected with ALMA, and contours are from 5$\sigma$ to the peak values in steps of 10$\sigma$.
+The bold gray lines represent the filament skeletons identified using H$^{13}$CO$^+$ as reported by zhou2022atoms. The green dashed rectangle is the area of the SiO emission maps where the SiO line profiles have been decomposed into different velocity components. The orange and blue rectangles, with the broadest and narrowest SiO line widths, respectively, indicate the locations where SiO and H$^{13}$CO$^+$ have been extracted.
+The field of view (FOV) is 72$^{\prime}^{\prime}$ corresponding with the FOV of the ALMA observations. All images have been primary-beam corrected. The source name and integrated velocity ranges (in km s$^{-1}$) are shown on the upper left and right corners, respectively. The beam size is reported in the lower left corner. The same images are provided for all sources within the supplementary material. (*fig3*)
+
+</div>
+<div id="div_fig3">
+
+<img src="tmp_2411.19489/./Figure/Figure5/SiO_velocity_final_report2.png" alt="Fig6.1" width="50%"/><img src="tmp_2411.19489/./Figure/Figure5/SiO_Width_final_report2.png" alt="Fig6.2" width="50%"/>
+
+**Figure 6. -** The histogram shows the velocity offset compared to the systemic velocity and line width distribution of the broad and narrow components of the SiO emission for the entire sample. The open blue histograms correspond to the sources without outflow activity, and the orange-filled histograms represent the sources exhibiting outflow activity. The outflow sources can be found in Table \ref{tab:TableA1}. (*fig5*)
+
+</div><div id="qrcode"><img src=https://api.qrserver.com/v1/create-qr-code/?size=100x100&data="https://arxiv.org/abs/2411.19489"></div>

docs/_build/html/2411.19686.md

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+
+<div id="title">
+
+#  MIRI Deep Imaging Survey (MIDIS) of the Hubble Ultra Deep Field$\thanks{Based on results from the MIRI European Consortium Guaranteed Time Observations, program 1283}$ : Project description and early results for the galaxy population detected at 5.6 $\mum$ 
+
+</div>
+<div id="comments">
+
+[![arXiv](https://img.shields.io/badge/arXiv-2411.19686-b31b1b.svg)](https://arxiv.org/abs/2411.19686)<mark>Appeared on: 2024-12-02</mark> -  _submitted to A&A on July 30, 2024_
+
+</div>
+<div id="authors">
+
+G. Östlin, et al. -- incl., <mark>F. Walter</mark>
+
+</div>
+<div id="abstract">
+
+**Abstract:** The recently launched James Webb Space Telescope (JWST) is opening new observing windows on the distant universe. Among JWST's instruments, the Mid Infrared Instrument (MIRI) offers the unique capability of imaging observations at wavelengths $\lambda > 5\mu$ m. This enables unique access to the rest frame near infra-red (NIR, $\lambda \ge 1$ $\mum$ ) emission from galaxies at redshifts $z>4$ and the visual ( $\lambda \gtrsim 5000$ Å) rest frame for $z>9$ . We here report on the guaranteed time observations (GTO) from the MIRI European Consortium, of the Hubble Ultra Deep Field (HUDF), forming the MIRI Deep Imaging Survey (MIDIS), consisting of an on source integration time of $\sim41$ hours in the MIRI/F560W (5.6 $\mu$ m) filter.   To our knowledge, this constitutes the longest single filter exposure obtained with JWST of an extragalactic field as yet. The HUDF is one of the most observed  extragalactic fields, with extensive multi-wavelength coverage, where (before  JWST) galaxies up to $z\sim 7$ have been  confirmed, and at $z>10$ suggested, from HST photometry. We aim to characterise the galaxy population in HUDF at 5.6 $\mu$ m, enabling studies such as: the rest frame NIR morphologies for galaxies at $z\lesssim4.6$ ,  probing mature stellar populations and emission lines  in $z>6$ sources, intrinsically red and dusty galaxies, and active galactic nuclei (AGN) and their host galaxies at intermediate redshifts. We have reduced the MIRI data using the $*JWST*$ pipeline, augmented by in-house custom scripts. We measure the noise characteristics of the resulting image. Galaxy photometry has been obtained, and photometric redshifts have been estimated for sources with available multi wavelength photometry (and compared to spectroscopic redshifts when available). Over the deepest part of our image  the 5 $\sigma$ point source limit is 28.65 mag AB (12.6 nJy), $\sim0.35$ mag better than predicted by the JWST exposure time calculator.   We find $\sim2500$ sources, the overwhelming majority of which are distant galaxies, but note that spurious sources likely remain at faint magnitudes due to imperfect cosmic ray rejection in the JWST pipeline.   More than 500 galaxies with available spectroscopic redshifts, up to $z\approx11$ have been identified, the majority of which are at $z<6$ .   More than 1000 galaxies have reliable photometric redshift estimates, of which $\sim25$ are  at $6<z<12$ .   The point spread function in the F560W filter has a FWHM of $\approx0.2\arcsec$ (corresponding to $1.4$ kpc at $z=4$ ), allowing the near infrared rest frame   morphologies  for the first time to be resolved up to $z\sim4$ . As expected, the  light distributions are smoother than at shorter wavelength, and trace the stellar mass distributions.    Moreover, $>100$ objects with very red  NIRCam vs MIRI (3.6--5.6 $\mum$ $>1$ ) colours have been found, indicating dusty or old stellar populations at high redshifts. We conclude that MIDIS  surpasses pre-flight expectations and that deep MIRI imaging has a great potential for characterizing the galaxy population from cosmic noon to dawn.
+
+</div>
+
+<div id="div_fig1">
+
+<img src="tmp_2411.19686/./Figures/midis_colordist_F356W-F560W_zcol.png" alt="Fig14" width="100%"/>
+
+**Figure 14. -** F560W magnitude vs NIRCAM/F356W--F560W color. Only sources with a F560W (F356W) magnitude uncertainty of 0.2 (0.5) or lower are included. The red circle indicates a confirmed MERO currently under investigation (Jermann et al. in prep). The colors indicate photometric redshift of the sources (gray points do not have a valid redshift estimate). (*color-mag*)
+
+</div>
+<div id="div_fig2">
+
+<img src="tmp_2411.19686/./Figures/hudf_mds_kron_err+hist.png" alt="Fig4" width="100%"/>
+
+**Figure 4. -** 
+   Top: F560W number counts for Kron magnitudes.
+   Bottom: F560W Kron magnitudes vs photometric uncertainty. The derived $5\sigma$ point source limiting magnitude is indicated by the dashed vertical line.  (*f560err+hist*)
+
+</div>
+<div id="div_fig3">
+
+<img src="tmp_2411.19686/./Figures/exptime_map_2col.png" alt="Fig9" width="100%"/>
+
+**Figure 9. -** Left: The F560W image with linear intensity scaling. Colored patches show regions where we have estimated the noise (see Table \ref{depthtable}) with different depths: the deepest area (A), where obs 1-2, 4-6 overlap (yellow). The deep area (B), where obs 4 does not overlap fully with the others (green). Outside these areas, there is coverage at less depth, notably the NE extension which only has observations from obs 4. The area with at least 7h of combined integration is denoted C (purple). The orientation is in the detector plane (x,y). Right: Exposure time map. (*image-exposuremap*)
+
+</div><div id="qrcode"><img src=https://api.qrserver.com/v1/create-qr-code/?size=100x100&data="https://arxiv.org/abs/2411.19686"></div>