-
Notifications
You must be signed in to change notification settings - Fork 0
Commit
This commit does not belong to any branch on this repository, and may belong to a fork outside of the repository.
- Loading branch information
1 parent
b303080
commit 2ef5275
Showing
13 changed files
with
793 additions
and
757 deletions.
There are no files selected for viewing
This file contains bidirectional Unicode text that may be interpreted or compiled differently than what appears below. To review, open the file in an editor that reveals hidden Unicode characters.
Learn more about bidirectional Unicode characters
| Original file line number | Diff line number | Diff line change |
|---|---|---|
| @@ -0,0 +1,105 @@ | ||
| <div class="macros" style="visibility:hidden;"> | ||
| $\newcommand{\ensuremath}{}$ | ||
| $\newcommand{\xspace}{}$ | ||
| $\newcommand{\object}[1]{\texttt{#1}}$ | ||
| $\newcommand{\farcs}{{.}''}$ | ||
| $\newcommand{\farcm}{{.}'}$ | ||
| $\newcommand{\arcsec}{''}$ | ||
| $\newcommand{\arcmin}{'}$ | ||
| $\newcommand{\ion}[2]{#1#2}$ | ||
| $\newcommand{\textsc}[1]{\textrm{#1}}$ | ||
| $\newcommand{\hl}[1]{\textrm{#1}}$ | ||
| $\newcommand{\footnote}[1]{}$ | ||
| $\newcommand{\cmnt}[1]$ | ||
| $\newcommand{\review}[1]{#1}$ | ||
| $\newcommand{\porb}{P_\mathrm{orb}}$ | ||
| $\newcommand{\pdot}{\dot{P}_\mathrm{orb}}$ | ||
| $\newcommand{\mdot}{\dot{M}}$ | ||
| $\newcommand{\teff}{T_\mathrm{eff}}$ | ||
| $\newcommand{\halpha}{H\alpha}$ | ||
| $\newcommand{\hbeta}{H\beta}$ | ||
| $\newcommand{\hei}{\ion{He}{I}}$ | ||
| $\newcommand{\heii}{\ion{He}{II}}$ | ||
| $\newcommand{\siii}{\ion{Si}{II}}$ | ||
| $\newcommand{\filus}{\textit{u_s}}$ | ||
| $\newcommand{\filgs}{\textit{g_s}}$ | ||
| $\newcommand{\filrs}{\textit{r_s}}$ | ||
| $\newcommand{\filis}{\textit{i_s}}$ | ||
| $\newcommand{\filzs}{\textit{z_s}}$ | ||
| $\newcommand{\filu}{\textit{u'}}$ | ||
| $\newcommand{\filg}{\textit{g'}}$ | ||
| $\newcommand{\filr}{\textit{r'}}$ | ||
| $\newcommand{\fili}{\textit{i'}}$ | ||
| $\newcommand{\filz}{\textit{z'}}$ | ||
| $\newcommand{\filkg}{\textit{KG5}}$ | ||
| $\newcommand{\inp}{{\tt input}}$ | ||
| $\newcommand{\beer}{{\tt beer}}$ | ||
| $\newcommand{\qmin}{{\tt qmin}}$ | ||
| $\newcommand{\mmmr}{{\tt mmmr}}$ | ||
| $\newcommand{\aell}{A_{\rm ell}}$ | ||
| $\newcommand{\qm}{q_{\rm min}}$ | ||
| $\newcommand{\fbh}{f_{\rm BH}}$ | ||
| $\newcommand{\sbar}{\Bar{S}'}$ | ||
| $\newcommand{\mpia}{1}$ | ||
| $\newcommand{\tlv}{2}$ | ||
| $\newcommand{\barilan}{3}$ | ||
| $\newcommand{\edin}{4}$ | ||
| $\newcommand{\caltech}{5}$ | ||
| $\newcommand{\ing}{6}$ | ||
| $\newcommand{\sheff}{7}$ | ||
| $\newcommand{\warw}{8}$</div> | ||
|
|
||
|
|
||
|
|
||
| <div id="title"> | ||
|
|
||
| # An upper limit on the frequency of short-period black hole companions to Sun-like stars | ||
|
|
||
| </div> | ||
| <div id="comments"> | ||
|
|
||
| [](https://arxiv.org/abs/2412.02082)<mark>Appeared on: 2024-12-04</mark> - _14 pages, 12 figures. Submitted to A&A. Comments welcome. Long forms of Tables 3 and 4 are included as FITS files in the Arxiv zip folder_ | ||
|
|
||
| </div> | ||
| <div id="authors"> | ||
|
|
||
| M. J. Green, et al. -- incl., <mark>H.-W. Rix</mark>, <mark>K. El-Badry</mark> | ||
|
|
||
| </div> | ||
| <div id="abstract"> | ||
|
|
||
| **Abstract:** Stellar-mass black holes descend from high-mass stars, most of which had stellar binary companions.However, the number of those binary systems that survive the binary evolution and black hole formation is uncertain by multiple orders of magnitude.The survival rate is particularly uncertain for massive stars with low-mass companions, which are thought to be the progenitors of most black hole X-ray binaries.We present a search for close black hole companions (separation $\lesssim 20 R_\odot$ ) to AFGK-type stars in _TESS_ , i.e. the non-accreting counterparts to and progenitors of low-mass X-ray binaries. Such black holes can be detected by the tidally induced ellipsoidal deformation of the visible star, and the ensuing photometric light-curve variations. From an initial sample of $4.7\times10^6$ TESS stars, we have selected 457 candidates for such variations. However, spectroscopic followup of 251 of them shows that none are consistent with a close black hole companion.On the basis of this non-detection, we determine ( $2\sigma$ confidence) that fewer than one in $10^5$ Solar-type stars in the Solar neighbourhood host a short-period black hole companion.This upper limit is in tension with a number of "optimistic" population models in the literature that predict short-period black hole companions around one in $\sim 10^{4-5}$ stars. Our limits are still consistent with other models that predict only a few in $\sim 10^{7-8}$ . | ||
|
|
||
| </div> | ||
|
|
||
| <div id="div_fig1"> | ||
|
|
||
| <img src="tmp_2412.02082/./figures/upperlim-2d/figure.png" alt="Fig8" width="100%"/> | ||
|
|
||
| **Figure 8. -** | ||
| Two-dimensional upper limits on the frequency of black hole companions to Solar-type stars as a function of orbital period and black hole mass, $f_{\rm BH} (M_2, P_{\rm orb})$. | ||
| The existence of orbital periods close to 1 day is more tightly constrained than the existence of periods close to 3 days. | ||
| Dark companions with masses $M_2 < 3 M_\odot$ are less tightly constrained than more massive companions, but above this limit the dependence on companion mass is weak. | ||
| $\cmnt${Is it true that high-mass bhs are harder to find at fixed period?} (*fig:upperlim-2d*) | ||
|
|
||
| </div> | ||
| <div id="div_fig2"> | ||
|
|
||
| <img src="tmp_2412.02082/./figures/gaia-confirmation/figure.png" alt="Fig6" width="100%"/> | ||
|
|
||
| **Figure 6. -** | ||
| The $K$-amplitudes derived via two methods from _Gaia_ data, against those measured from orbital solutions, for all targets with both measurements. | ||
| There is generally reasonable agreement, with some outlying points, as discussed in the text. | ||
| (*fig:rv-comparison*) | ||
|
|
||
| </div> | ||
| <div id="div_fig3"> | ||
|
|
||
| <img src="tmp_2412.02082/./figures/selection-functions/figure.png" alt="Fig9" width="100%"/> | ||
|
|
||
| **Figure 9. -** | ||
| Probability for simulated binary systems of various types to be accepted into the $\beer$ sample (top), $\qmin$ sample (middle), and $\mmmr$ sample (bottom), as a function of period. | ||
| Other variables ($\cos i$, $M_1$, and $M_2$) have been marginalised over. | ||
| (*fig:selection-function-beer*) | ||
|
|
||
| </div><div id="qrcode"><img src=https://api.qrserver.com/v1/create-qr-code/?size=100x100&data="https://arxiv.org/abs/2412.02082"></div> |
This file contains bidirectional Unicode text that may be interpreted or compiled differently than what appears below. To review, open the file in an editor that reveals hidden Unicode characters.
Learn more about bidirectional Unicode characters
| Original file line number | Diff line number | Diff line change |
|---|---|---|
| @@ -0,0 +1,74 @@ | ||
| <div class="macros" style="visibility:hidden;"> | ||
| $\newcommand{\ensuremath}{}$ | ||
| $\newcommand{\xspace}{}$ | ||
| $\newcommand{\object}[1]{\texttt{#1}}$ | ||
| $\newcommand{\farcs}{{.}''}$ | ||
| $\newcommand{\farcm}{{.}'}$ | ||
| $\newcommand{\arcsec}{''}$ | ||
| $\newcommand{\arcmin}{'}$ | ||
| $\newcommand{\ion}[2]{#1#2}$ | ||
| $\newcommand{\textsc}[1]{\textrm{#1}}$ | ||
| $\newcommand{\hl}[1]{\textrm{#1}}$ | ||
| $\newcommand{\footnote}[1]{}$ | ||
| $\newcommand{\tabularfootnotes}{$ | ||
| $ \setcounter{savedfootnote}{\value{footnote}}$ | ||
| $ \setcounter{footnote}{0}$ | ||
| $ \newcommand{\thefootnote}{\textit{\arabic{footnote}}}$ | ||
| $}$ | ||
| $\newcommand{\restorefootnotes}{$ | ||
| $ \setcounter{footnote}{\value{savedfootnote}}$ | ||
| $ \newcommand{\thefootnote}{\arabic{footnote}}$ | ||
| $}$ | ||
| $\newcommand{\arraystretch}{1.5}$ | ||
| $\newcommand{\epsilon}{\varepsilon}$ | ||
| $\newcommand{\thefootnote}{\textit{\arabic{footnote}}}$ | ||
| $\newcommand{\thefootnote}{\arabic{footnote}}$ | ||
| $\newcommand\cigale{{{\sc cigale}}}$ | ||
| $\newcommand\microns{{ \mum}}$ | ||
| $\newcommand\HI{{H{\sc i}}}$ | ||
| $\newcommand\HInewcommand{{H{\sc i}-newcommand}}$</div> | ||
|
|
||
|
|
||
|
|
||
| <div id="title"> | ||
|
|
||
| # Dust emission from the bulk of galaxies at the Epoch of Reionization | ||
|
|
||
| </div> | ||
| <div id="comments"> | ||
|
|
||
| [](https://arxiv.org/abs/2412.02557)<mark>Appeared on: 2024-12-04</mark> - _Submitted to A&A_ | ||
|
|
||
| </div> | ||
| <div id="authors"> | ||
|
|
||
| L. Ciesla, et al. -- incl., <mark>E. Schinnerer</mark> | ||
|
|
||
| </div> | ||
| <div id="abstract"> | ||
|
|
||
| **Abstract:** The excess of UV bright galaxies observed at $z>10$ has been one of the major surprises from the JWST early observations.Several explanations have been proposed to understand the mild change in space density of the UV bright galaxies at these high redshifts, among them an evolution of dust attenuation properties in galaxies.However, our view of dust in primordial galaxies is limited towards a few tens of $z\sim7$ galaxies, pre-selected from UV-optical observations, and are thus not necessarily representative of the bulk of the sources at these redshifts.In this work, we aim at constraining the dust properties of galaxies at $6<z<12$ by making the most of the A $^3$ COSMOS database in the JADES/GOODS-South field.We stacked ALMA band 6 and 7 observations of 4464 JADES galaxies covered by the A $^3$ COSMOS database and used the measurements as constraints to perform UV-to-FIR SED modelling.We obtain tentative signals for the brightest UV galaxies ( $M_{\mathrm{UV}}<-19$ mag) as well as for the most massive ones ( $\log M_\star/M_\odot>9$ ) at $6<z<7$ , and upper limits for fainter ( $M_{\mathrm{UV}}>-19$ mag), lower mass sources ( $\log M_\star/M_\odot<9$ ), and at higher redshift ( $z>7$ ).Fitting these $6<z<7$ galaxies with ALMA constraints results in lower star formation rates ( $-0.4$ dex) and FUV attenuation ( $-0.5$ mag) for galaxies with $\log M_\star/M_\odot>8$ , compared to the fit without FIR.We extend the $L_{\mathrm{IR}}$ vs $M_{\mathrm{UV}}$ relation down to $M_{\mathrm{UV}}=-19$ mag and show a tentative breakdown of the relation at fainter UV magnitudes.The positions of the JADES $z\sim6.5$ sample on the infrared excess (IRX) versus $\beta$ and IRX versus $M_\star$ diagrams are consistent with those of the ALPINE ( $z\sim5.5$ ) and REBELS ( $z\sim6.5$ ) samples, suggesting that the dust composition and content of our mass-selected sample are similar to these UV-selected galaxies.Extending our analysis of the infrared properties to $z>7$ galaxies, we find a non-evolution of $\beta$ in the $M_{\mathrm{UV}}$ range probed by our sample (-17.24 $^{+0.54}_{-0.62}$ ) and highlight the fact that samples from the literature are not representative of the bulk of galaxy populations at $z>6$ .We confirm a linear relation between A $_{\rm V}$ and sSFR $^{-1}$ with a flatter slope than previously reported due to the use of ALMA constraints.Our results suggest that rapid and significant dust production has already happened by $z\sim7$ . | ||
|
|
||
| </div> | ||
|
|
||
| <div id="div_fig1"> | ||
|
|
||
| <img src="tmp_2412.02557/./lir_muv.png" alt="Fig4" width="100%"/> | ||
|
|
||
| **Figure 4. -** Infrared luminosity as a function of UV magnitude. The contours show the position of the whole sample with $L_{\mathrm{IR}}$ obtained from the fit using the ALMA constraint. Big circles with black borders are the weighted median values in four UV magnitude bins. Stacked or median values for samples from the literature are show in various shades of blue symbols \citep{Bowler24,Khusanova21}. (*fig:lir_muv*) | ||
|
|
||
| </div> | ||
| <div id="div_fig2"> | ||
|
|
||
| <img src="tmp_2412.02557/./LIR_lowT_MUV_full.png" alt="Fig7" width="100%"/> | ||
|
|
||
| **Figure 7. -** $L_{\mathrm{IR}}$ distributions of galaxies in the four UV magnitude bins considered in this work, assuming different dust temperatures. (*fig:lir_muv_lowT*) | ||
|
|
||
| </div> | ||
| <div id="div_fig3"> | ||
|
|
||
| <img src="tmp_2412.02557/./lir_redshift.png" alt="Fig10" width="100%"/> | ||
|
|
||
| **Figure 10. -** IR luminosity as a function of redshift for our sample (black contours, downward arrows indicate upper limits) and different samples from the literature \citep[shades of blue,][]{Laporte17,Laporte19,Tamura19,Inami22,Mitsuhashi24,Schouws24}. Symbols with downward arrows are upper limits. Circles with black border are our fiducial UV magnitude bins. (*fig:lirz*) | ||
|
|
||
| </div><div id="qrcode"><img src=https://api.qrserver.com/v1/create-qr-code/?size=100x100&data="https://arxiv.org/abs/2412.02557"></div> |
This file contains bidirectional Unicode text that may be interpreted or compiled differently than what appears below. To review, open the file in an editor that reveals hidden Unicode characters.
Learn more about bidirectional Unicode characters
This file contains bidirectional Unicode text that may be interpreted or compiled differently than what appears below. To review, open the file in an editor that reveals hidden Unicode characters.
Learn more about bidirectional Unicode characters
This file contains bidirectional Unicode text that may be interpreted or compiled differently than what appears below. To review, open the file in an editor that reveals hidden Unicode characters.
Learn more about bidirectional Unicode characters
Oops, something went wrong.