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+ +# A SPectroscopic survey of biased halos In the Reionization Era (ASPIRE): \ Spectroscopically Complete Census of Obscured Cosmic Star Formation Rate Density at $z=4-6$ + +
+
+ +[![arXiv](https://img.shields.io/badge/arXiv-2412.06894-b31b1b.svg)](https://arxiv.org/abs/2412.06894)Appeared on: 2024-12-11 - _27 pages, 13 figures, 3 tables. Accepted for publication in ApJ_ + +
+
+ +F. Sun, et al. -- incl., Y. Khusanova, F. Walter + +
+
+ +**Abstract:** We present a stringent measurement of the dust-obscured star-formation rate density (SFRD) at $z=4-6$ from the ASPIRE JWST Cycle-1 medium and ALMA Cycle-9 large program.We obtained JWST/NIRCam grism spectroscopy and ALMA 1.2-mm continuum map along 25 independent quasar sightlines, covering a total survey area of $\sim$ 35 arcmin $^2$ where we search for dusty star-forming galaxies (DSFGs) at $z = 0 - 7$ .We identify eight DSFGs in seven fields at $z=4-6$ through the detection of $\ha$ or $\oiii$ $\lambda$ 5008 lines, including fainter lines such as $\hb$ , $\oiii$ $\lambda$ 4960, $\nii$ $\lambda$ 6585, $\sii$ $\lambda\lambda$ 6718,6733 for six sources.With this spectroscopically complete DSFG sample at $z=4-6$ and negligible impact from cosmic variance (shot noise), we measure the infrared luminosity function (IRLF) down to $L_\mathrm{IR} \sim 2\times10^{11}$ $\lsun$ .We find flattening of IRLF at $z=4-6$ towards the faint end (power-law slope $\alpha = 0.59_{-0.45}^{+0.39}$ ).We determine the dust-obscured cosmic SFRD at this epoch as $\log[\rho_\mathrm{SFR,IR} / (\mathrm{M}_\odot \mathrm{yr}^{-1} \mathrm{Mpc}^{-3})] = -1.52_{-0.13}^{+0.14}$ .This is significantly higher than previous determination using ALMA data in the Hubble Ultra Deep Field, which is void of DSFGs at $z=4-6$ because of strong cosmic variance (shot noise).We conclude that the majority ( $66\pm7$ \% ) of cosmic star formation at $z \sim 5$ is still obscured by dust.We also discuss the uncertainty of SFRD propagated from far-IR spectral energy distribution and IRLF at the bright end, which will need to be resolved with future ALMA and JWST observations. + +
+ +
+ +Fig4 + +**Figure 4. -** 1.2-mm continuum images of 25 quasar fields obtained by ASPIRE ALMA Cycle-9 large program. In the top-left panel, we highlight the design of JWST/NIRCam and ALMA observations. +The whole ALMA 1.2-mm continuum imaging mosaics (_uv_-tapered with FWHM = 1$\arcsec$) are within the full spectral ($\lambda$ = 3.1--4.0 $\micron$ with F356W filter) coverage region of NIRCam module A as indicated by the blue shaded region. +The quasar J0109--3047 ($z=6.791$; cyan circle) is located in the center of ALMA footprint, and one DSFG (J0109m3047.C02 at $z=5.549$) is also highlighted with red circle. +The position angle of NIRCam WFSS observation is 270\arcdeg for J0109 field, and therefore the grism-R dispersion direction is almost from north to south as indicated by the orange arrow. +Note that the dispersion direction depends on the JWST/NIRCam PA and varies from field to field. +ALMA 1.2-mm continuum images of all the other 24 fields are also displayed. Quasars with continuum detection ($z=6.5-6.8$) and spectroscopically confirmed DSFGs at $z=4-6$ are highlighted in cyan and red circles, respectively. +Many DSFGs at other redshifts are also detected with ALMA but not highlighted in this figure. + (*fig:all_alma*) + +
+
+ +Fig3 + +**Figure 3. -** Completeness as a function of ALMA flux density on 1$\farcs$0 _uv_-tapered images (before primary beam response correction). +Best-fit error function is shown as the solid black line. + (*fig:complete*) + +
+
+ +Fig5 + +**Figure 5. -** JWST NIRCam (red: F356W; green: F200W, blue: F115W) and ALMA 1.2-mm continuum images of DSFGs at $z=4-6$ discovered with the ASPIRE survey. Image sizes are 4$\arcsec$$\times$4$\arcsec$(north up, east left). +Source ID, spectroscopic redshifts and ALMA beam sizes are indicated in the plots. +Most sources appear red in JWST RGB images, indicating that they are highly dust-obscured galaxies at high redshifts. +Note that J0109m3047.C02 is gravitationally lensed by the bright galaxy on the left (see Appendix \ref{apd:01_lens}). + (*fig:cutout*) + +
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+ +# Little iLocater: paving the way for iLocater + +
+
+ +[![arXiv](https://img.shields.io/badge/arXiv-2412.06897-b31b1b.svg)](https://arxiv.org/abs/2412.06897)Appeared on: 2024-12-11 - _13 pages, 17 figures, accepted for publication in MNRAS_ + +
+
+ +R. J. Harris, et al. -- incl., S. Barboza + +
+
+ +**Abstract:** Diffraction-limited radial velocity instruments offer a pathway towards improved precision and stability, and the exploration of new parameter spaces at high spatial and spectral resolution. However, achieving the necessary performance requires careful instrument design and considerable on-sky testing. We describe the design and construction of "Little iLocater" (Lili), a compact spectrograph that has been used to validate the performance of the front-end fibre-injection system of the iLocater spectrograph. We present the design, assembly, and performance using on-sky data obtained at the Large Binocular Telescope (LBT), including extraction of spectra from standard stars, testing of the atmospheric dispersion corrector to elevations of $\qty{40}{◦ee}$ , and spatially resolved spectra from close companion systems. These results show the front-end fibre-injection system is performing as expected and is indicative of iLocater's capabilities once installed at the LBT. + +
+ +
+ +Fig1 + +**Figure 1. -** Shaded rendering of the optical design of the \ac{Lili} spectrograph, with the light path coloured by wavelength. From left to right, the light from the \ac{SMF} is collimated by an \ac{OAP}, which feeds a \ac{VPH} grating. Light is then refocused onto the detector by a TTL200-S8 and AC-508-080-C lens. (*fig:Lili_optical_design*) + +
+
+ +Fig5 + +**Figure 5. -** Estimated spectrograph throughput based on commercially available values for lenses and theoretical values for the \ac{MCIFU} gratings. Individual efficiencies of the two spectrograph orders are plotted as dotted lines. The filled area underneath indicates the parts of the spectrum from each order incident on the \ac{CRED2} detector. (*fig:Lili_transmission*) + +
+
+ +Fig3 + +**Figure 3. -** Footprint of the two orders imaged onto the detector. The first order (\qtyrange{0.97}{1.2}{\micro\meter}) crosses the full detector area diagonally, while the second sits below (\qtyrange{1.2}{1.34}{\micro\meter}). Note that there is a difference in slope between the first and second orders due to the rotation of the diffraction gratings. (*fig:Lili_footprint*) + +
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+ +# Pushing ALMA to the limit: 140 pc resolution observations of a z=6.6 quasar-galaxy merger resolve strikingly different morphologies of dust continuum and [$\ion{C}{2}$] 158$\mu\rm{m}$ emission + +
+
+ +[![arXiv](https://img.shields.io/badge/arXiv-2412.07474-b31b1b.svg)](https://arxiv.org/abs/2412.07474)Appeared on: 2024-12-11 - _Accepted in ApJ. 15 pages + appendices_ + +
+
+ +R. A. Meyer, et al. -- incl., F. Walter + +
+
+ +**Abstract:** We present $0\farcs026$ $(140 \rm{pc})$ resolution ALMA observations of [ $\ion{C}{2}$ ] $158 \mu\rm{m}$ and dust continuum emission of the $z=6.6$ quasar J0305--3150, resolved over $\sim 300-400$ independent resolution elements. The dust continuum emission is compact with $\sim 80\%$ recovered within $r<0\farcs3$ $(1.6 \rm{kpc})$ , whereas the [ $\ion{C}{2}$ ] emission profile is composed of a central Gaussian ( $r<0\farcs4$ , i.e. $<2.2 \rm{kpc}$ ) and an extended component (detected up to $\sim 10 \rm{kpc}$ at $>3\sigma$ ). We infer a direct contribution of the quasar to the observed 260 $\rm{GHz}$ continuum $S_{\nu,\rm{QSO}} / S_{\nu,\rm{QSO+Host}} \lesssim 1\%$ . We report the detection of FIR-detected star-forming clumps with $r<200 \rm{pc}$ and properties similar to that of rest-frame UV-optical clumps reported in the literature.The $200 \rm{pc}$ resolved [ $\ion{C}{2}$ ] /FIR ratio follows the global relation with the FIR surface brightness established in low- and high-redshift galaxies, even at the quasar location.We find that dust continuum is emitted in regions of $\sim0\farcs02-0\farcs04$ consistent with the size of photo-dissociation regions (PDR), whereas $50\%$ of the [ $\ion{C}{2}$ ] originates from larger physical scales ( $\theta \gtrsim 2"$ ). The large-scale [ $\ion{C}{2}$ ] emission presents a velocity gradient aligned with a nearby companion with perturbed kinematics, and misaligned with the kinematics of the small-scale emission. The absence of significant [ $\ion{C}{2}$ ] emission by structures with physical scale $\lesssim 1 \rm{kpc}$ implies that [ $\ion{C}{2}$ ] emission is not produced in dense PDR located at the boundary of Giant Molecular Clouds. We argue instead that [ $\ion{C}{2}$ ] is produced in low-density PDRs in the interstellar medium and diffuse $\ion{H}{1}$ gas tidally-stripped during the ongoing merger. + +
+ +
+ +Fig9 + +**Figure 9. -** Top: FIR continuum at $\sim 260 \rm{GHz}$ and velocity-integrated [$\ion${C}{2}] emission of the high--redshift quasar J0305--3150, based on all available ALMA observations, including earlier ‘lower'--resolution data published by Venemans2016, Venemans2019. The contours start at $\pm2\sigma$ and increase in powers of two. Positive contours are shown in full dark lines, and negative ones in dashed grey. The synthesized beam is plotted in the bottom left corner of each plot. The GAIA-corrected optical position of the quasar is shown with a star \citep[][]{Venemans2019}. Bottom: Mean velocity and velocity dispersion map of the [$\ion${C}{2}] emission, computed using a Gaussian fit in pixels where [$\ion${C}{2}] is detected at $>2\sigma$. The mask for the moment 1 and 2 maps is given by the moment 0 $2\sigma$ contours, with five rounds of binary erosion and binary dilation to remove small structures due to noise (see text for more details). (*fig:fig1*) + +
+
+ +Fig3 + +**Figure 3. -** Star-formation rate density ($\Sigma_{\rm{SFR}}$) map of J0305--3150 assuming a proportional relation between the dust emission and the $\Sigma_{\rm{SFR}}$. The contours start at $\pm2\sigma$ and increase in steps of $2\sigma$(up to $8\sigma$ only). The synthesized beam is plotted in the bottom left corner. The gray box shows the area tessellated with independent $r=0$\farcs$037 (200 \rm{pc}$ apertures used to study the resolved FIR properties (see further text and Fig. \ref{fig:resolved_CII_deficit}. The cyan circles show $r=0$\farcs$037$ apertures corresponding to regions of interest (see further text and Table \ref{tab:clumps_properties}). (*fig:sfrd_map*) + +
+
+ +Fig10 + +**Figure 10. -** **Left panel:** Real part of the visibilities for the continuum and [$\ion${C}{2}] emission, averaged as a function of baseline length converted to physical scales. The errorbars represent the standard deviation in each bin, and the visibilities are normalised to the first datapoint (_uv_ distances $(15\pm1)\rm{m}$). The best-fit cumulative distribution functions are shown in dashed black. **Right panel:** Best-fit probability density function for the continuum and [$\ion${C}{2}] emission as a function of the logarithm of the physical scale observed. The maximum recoverable scale of the ALMA C10 observations is shown in dashed black. We also indicate the photo-dissociation regions (PDR) sizes where [$\ion${C}{2}] is thought to originate found in simulations and observations at $0\lesssim z\lesssim 5$(black markers and errors), and provide a similar estimate for J0305--3150 in dark red. \nocite{Carlstrom1991} (*fig:visiblities_scales*) + +
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+ +# The CARMENES search for exoplanets around M dwarfs: The impact of rotation and magnetic fields on the radial velocity jitter in cool stars + +
+
+ +[![arXiv](https://img.shields.io/badge/arXiv-2412.07691-b31b1b.svg)](https://arxiv.org/abs/2412.07691)Appeared on: 2024-12-11 - + +
+
+ +H. L. Ruh, et al. -- incl., T. Henning + +
+
+ +**Abstract:** Radial velocity (RV) jitter represents an intrinsic limitation on the precision of Doppler searches for exoplanets that can originate from both instrumental and astrophysical sources. We aim to determine the RV jitter floor in M dwarfs and investigate the stellar properties that lead to RV jitter induced by stellar activity. We determined the RV jitter in $\num{239}$ M dwarfs from the CARMENES survey that are predominantly of mid to late spectral type and solar metallicity. We also investigated the correlation between stellar rotation and magnetic fields with RV jitter. The median jitter in the CARMENES sample is $\SI{3.1}{\meter\per\second}$ , and it is $\SI{2.3}{\meter\per\second}$ for stars with an upper limit of $\SI{2}{\kilo\meter\per\second}$ on their projected rotation velocities. We provide a relation between the stellar equatorial rotation velocity and RV jitter in M dwarfs based on a subsample of $\num{129}$ well-characterized CARMENES stars. RV jitter induced by stellar rotation dominates for stars with equatorial rotation velocities greater than $\SI{1}{\kilo\meter\per\second}$ . A jitter floor of $\SI{2}{\meter\per\second}$ dominates in stars with equatorial rotation velocities below $\SI{1}{\kilo\meter\per\second}$ . This jitter floor likely contains contributions from stellar jitter, instrumental jitter, and undetected companions. We study the impact of the average magnetic field and the distributions of magnetic filling factors on the RV jitter. We find a series of stars with excess RV jitter and distinctive distributions of magnetic filling factors. These stars are characterized by a dominant magnetic field component between $\SIrange{2}{4}{\kilo\gauss}$ . An RV jitter floor can be distinguished from RV jitter induced by activity and rotation based on the stellar equatorial rotation velocity. RV jitter induced by activity and rotation primarily depends on the equatorial rotation velocity. This RV jitter is also related to the distribution of magnetic filling factors, and this emphasizes the role of the magnetic field in the generation of RV jitter. + +
+ +
+ +Fig4 + +**Figure 4. -** Jitter-rotation relation for \num{129} CARMENES M dwarfs with known rotation periods. The RV jitter is fit as a function of the stellar rotation velocity $v_{\rm eq}$. The solid line displays the best fit, and the shaded region indicates the prediction interval. The jitter floor and the linear trend (dashed lines) correspond to parameters $\alpha$ and $\beta$ in Eq. (\ref{eq:jitter_vrot}). (*fig:jitter_vrot_all*) + +
+
+ +Fig6 + +**Figure 6. -** Radial velocity jitter vs. mean magnetic field. The upper limits on the average magnetic field are indicated by triangles. (*fig:jitter_bfield*) + +
+
+ +Fig9 + +**Figure 9. -** As Fig. \ref{fig:jitter_vrot_all}, but color-coded with the filling factor distributions index and only for stars with measured average magnetic field. The labels mark the series of high-jitter stars with concentrated magnetic field distributions. The empty circles display stars without measurements of the average magnetic field. (*fig:bfield_structure*) + +
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