Datasets:
ReadingTimeMachine
/
rtm-sgt-ocr-v1

Dataset card Data Studio Files Community
1
source
stringlengths
1
2.05k
⌀
target
stringlengths
1
11.7k
. Similarly. the close passage of the source to a cusp could in principle give rise to finite source effects1994).. as for example was recently observed in the case ofcitepebO5.
Similarly, the close passage of the source to a cusp could in principle give rise to finite source effects, as for example was recently observed in the case of.
. Indeed. the combination of parallax and finite-source effects permitted to measure the mass of a microlens for the first time.
Indeed, the combination of parallax and finite-source effects permitted to measure the mass of a microlens for the first time.
We have therefore searched for both parallax and finite source effects. but find no significant detection of either.
We have therefore searched for both parallax and finite source effects, but find no significant detection of either.
Finally. we examine the position of the source on the color-magnitude diagram (CMD: Fig. 4 3)).
Finally, we examine the position of the source on the color-magnitude diagram (CMD; Fig. \ref{fig:cmd}) ).
The most prominent feature found in the CMD ts a track of stars running diagonally in the same direction as would the main sequence.
The most prominent feature found in the CMD is a track of stars running diagonally in the same direction as would the main sequence.
Since the field is in the Galactic disk. this feature is probably not a true maim sequence. but rather likely to be a “reddening sequence". that ts. an ensemble of mostly disk turnoff stars at progressively greater distances and correspondingly greater reddenings.
Since the field is in the Galactic disk, this feature is probably not a true main sequence, but rather likely to be a “reddening sequence”, that is, an ensemble of mostly disk turnoff stars at progressively greater distances and correspondingly greater reddenings.
The baseline “star” (combined light of the source and blended light) lies within this sequence toward its faint/red end although its position is seeing-dependent because of the seeing-correction term.
The baseline “star” (combined light of the source and blended light) lies within this sequence toward its faint/red end although its position is seeing-dependent because of the seeing-correction term.
The position indicated in the CMD is plotted assuming median seeing.
The position indicated in the CMD is plotted assuming median seeing.
However. the source itself [7,=20.9. (V.T),= 1.91] lies ~2mag below the baseline “star” in a region of the CMD that is well below the threshold of detection.
However, the source itself $I_{\rm s}=20.9$, $(V-I)_{\rm s}=1.94$ ] lies $\sim 2\ \mbox{mag}$ below the baseline “star,” in a region of the CMD that is well below the threshold of detection.
If the baseline were mainly composed of source light. and the "blended light" were simply source light that had been falsely attributed to blending by a wrong model. then the real source would lie within the well populated “reddening sequence". and the timescale would be much shorter. fe~30days.
If the baseline were mainly composed of source light, and the “blended light” were simply source light that had been falsely attributed to blending by a wrong model, then the real source would lie within the well populated “reddening sequence”, and the timescale would be much shorter, $t_{\rm E}\sim 30\ \mbox{days}$.
We therefore searched for solutions with little or no blending.
We therefore searched for solutions with little or no blending.
However. we find that these are ruled out with A4?= 2110.
However, we find that these are ruled out with $\Delta\chi^2=2440$ .
Furthermore. the best-fit models with no blended light are still extreme-separation binaries and not planetary systems.
Furthermore, the best-fit models with no blended light are still extreme-separation binaries and not planetary systems.
Since we have only a crude understanding of the CMD. no strong
Since we have only a crude understanding of the CMD, no strong
intterior structure 1s expected to occur in late A-type stars.
terior structure is expected to occur in late A-type stars.
scalings obtained with the mixing model are in excellent agreement with observations.
scalings obtained with the mixing model are in excellent agreement with observations.
The model also explains the observed discontinuitv in cluster properties al AZ~1—2 keV as a consequence of (he change in the cooling function at this temperature. aud provides a natural explanation lor the eitvopy floor seen in galaxy groups.
The model also explains the observed discontinuity in cluster properties at $kT\sim1-2$ keV as a consequence of the change in the cooling function at this temperature, and provides a natural explanation for the entropy floor seen in galaxy groups.
These results. (hough not inconsistent wilh some of the previously proposed explanations (see references in 844). suggest that those models should be gejeralized to include (he effect of turbulent heat transport.
These results, though not inconsistent with some of the previously proposed explanations (see references in 4), suggest that those models should be generalized to include the effect of turbulent heat transport.
After this paper was submitted to the journal. Voiet Fabian posted a paper (astro- in whic1 they have suggested independently that turbulent heat transport may be important in egalaxv clusters.
After this paper was submitted to the journal, Voigt Fabian posted a paper (astro-ph/0308352) in which they have suggested independently that turbulent heat transport may be important in galaxy clusters.
The authors thank Nadia Zakamska and Larry David [or providing the cluster data shown in Figure 1. ancl the referee for helpful comments.
The authors thank Nadia Zakamska and Larry David for providing the cluster data shown in Figure 1, and the referee for helpful comments.
This work was supported in part bv NASA gerant. NAC15-LOTSO ancl NSF grant. AST 0307433.
This work was supported in part by NASA grant NAG5-10780 and NSF grant AST 0307433.
due to long wavelength WIL instabilities has only a weak dependence on the shock Mach. number.
due to long wavelength KH instabilities has only a weak dependence on the shock Mach number.
One finds that (xu=2465, when M= L5. and (gy=1.921 when Al=40.
One finds that $t_{\rm KH} = 2.4 \,t_{\rm cc}$ when $M=1.5$ , and $t_{\rm KH} = 1.33 \,t_{\rm cc}$ when $M=40$.
These estimates are roughly 6 times shorter than the numerically determined. lifetimes at high. shock Mach number (AZz 7).
These estimates are roughly 6 times shorter than the numerically determined lifetimes at high shock Mach number $M\gtsimm 7$ ).
The scaling of the cloucl lifetime (in units of £f.) with AZ is also weaker than is observed from. the simulations (see Fig. 18)).
The scaling of the cloud lifetime (in units of $t_{\rm cc}$ ) with $M$ is also weaker than is observed from the simulations (see Fig. \ref{fig:massloss}) ).
For instance. it prediets that the lifetime of a cloud hit by a Mach. 1.5 shock is about 15 times longer than in a Mach 40 interaction.
For instance, it predicts that the lifetime of a cloud hit by a Mach 1.5 shock is about 1.8 times longer than in a Mach 40 interaction.
Nonetheless. the insensitivity of Eq.
Nonetheless, the insensitivity of Eq.
12. to the cloud. density contrast. v. is consistent with the numerical results. where only a weak (and non-montonic) dependence is seen (Fig. 18)).
\ref{eq:kh_destruction_time} to the cloud density contrast, $\chi$, is consistent with the numerical results, where only a weak (and non-montonic) dependence is seen (Fig. \ref{fig:massloss}) ).
Given these observations. it seems. reasonable to associate the mode of cloud destruction with ΙΝΕ instabilities. but it is clear that the lifetime of the cloud. fig.cGly.
Given these observations, it seems reasonable to associate the mode of cloud destruction with KH instabilities, but it is clear that the lifetime of the cloud, $t_{\rm life} \sim 6\,t_{\rm KH}$.
This expression is within a factor of 2 or so of the numerically determined lifetime of clouds with 10«X107 hit by shocks with AJ21.5. with the biggest discrepancy at low Alach numbers.
This expression is within a factor of 2 or so of the numerically determined lifetime of clouds with $10 < \chi < 10^{3}$ hit by shocks with $M > 1.5$, with the biggest discrepancy at low Mach numbers.
Ehe parameters of the fits to the numerical results are noted in Table 6..
The parameters of the fits to the numerical results are noted in Table \ref{tab:tlifefits}.
This is the second. of a series of papers investigating the turbulent destruction of clouds.
This is the second of a series of papers investigating the turbulent destruction of clouds.
In our first paper (Pittareetal.2009) the focus was primarily on the much faster evolution and dispersal of a cloud over-run by a shock with a highly turbulent post-shock llow.
In our first paper \citep{Pittard:2009} the focus was primarily on the much faster evolution and dispersal of a cloud over-run by a shock with a highly turbulent post-shock flow.
Here we have performed a detailed examination of the Mach number dependence of the destruction of a cloud by an adiabatic shock.
Here we have performed a detailed examination of the Mach number dependence of the destruction of a cloud by an adiabatic shock.
We have used. ahyvedrodynamical code which incorporates a sub-grid compressible &- turbulence model in an attempt to calculate
We have used ahydrodynamical code which incorporates a sub-grid compressible $k$ $\epsilon$ turbulence model in an attempt to calculate
A.
.
. This might weaken the rotating cloud interpretation.
This might weaken the rotating cloud interpretation.
Furthermore. Figs.
Furthermore, Figs.
4. and 6 show that only molecular gas at more negative velocities (~ —27 4 -26 )) coincide with3503... which suggests that the velocity gradient might be a direct consequence of an interaction between clump A and.
\ref{fig:pos-vel} and \ref{fig:mosaico1} show that only molecular gas at more negative velocities $\sim$ $-$ 27 / $-$ 26 ) coincide with, which suggests that the velocity gradient might be a direct consequence of an interaction between clump A and.
. Therefore. although rotation can not be entirely ruled out with the present data. we consider different origins for the velocity gradient observed across clump A. namely. 1) the expansion of the nebula at ~ 5 (see Sect 4.1) has been accumulating molecular gas behind the shock front which originated the expansion of clump A at approximately the same velocity of the ionized gas. as expected according to the models of ?.. 2) the velocity gradient of clump A is the consequence of a collision between Component | and another molecular cloud. which in turn. might have induced the formation of Pis 17 and the candidate YSOs reported in Sect.
Therefore, although rotation can not be entirely ruled out with the present data, we consider different origins for the velocity gradient observed across clump A, namely, 1) the expansion of the nebula at $\sim$ 5 (see Sect 4.1) has been accumulating molecular gas behind the shock front which originated the expansion of clump A at approximately the same velocity of the ionized gas, as expected according to the models of \citet{hi96}, 2) the velocity gradient of clump A is the consequence of a collision between Component 1 and another molecular cloud, which in turn, might have induced the formation of Pis 17 and the candidate YSOs reported in Sect.
3.3.
3.3.
Although they are rare. cloud-cloud collisions can lead to gravitational instabilities in the dense. shocked gas. resulting in triggered star formation (see 9?.. and references therein). 3) clump A is actually composed by different subclumps at different velocities. which are not resolved by the NANTEN observations.
Although they are rare, cloud-cloud collisions can lead to gravitational instabilities in the dense, shocked gas, resulting in triggered star formation (see \citealt{elm98}, and references therein), 3) clump A is actually composed by different subclumps at different velocities, which are not resolved by the NANTEN observations.
In this case. might be related with a subclump at more negative velocities.
In this case, might be related with a subclump at more negative velocities.
Further high-resolution studies with instruments like APEX may help to clarify this question.
Further high-resolution studies with instruments like APEX may help to clarify this question.
As mentioned in Sect 3.1.2. clump A exhibits an excitation temperatureK.. which is also the highest excitation temperature along Component |.
As mentioned in Sect 3.1.2, clump A exhibits an excitation temperature, which is also the highest excitation temperature along Component 1.
This temperature is higher than expected inside molecular cores if only cosmic ray ionization is considered as the main heating source2)... which implies that additional heating processes are present close to clump A. Very likely. clump A is being externally heated through the phototonisation of its surface layers (2). as a consequence of its proximity to.
This temperature is higher than expected inside molecular cores if only cosmic ray ionization is considered as the main heating source, which implies that additional heating processes are present close to clump A. Very likely, clump A is being externally heated through the photoionisation of its surface layers \citep{U09} as a consequence of its proximity to.
. This scenario is in line with the presence of the PDR at the interface between and clump A (see 3.3)).
This scenario is in line with the presence of the PDR at the interface between and clump A (see ).
In this context. it would be instructive to make a simple comparison of the PDR dust surface temperature. with the dust temperature obtained before towards the edge of (see Fig.9)).
In this context, it would be instructive to make a simple comparison of the PDR dust surface temperature, with the dust temperature obtained before towards the edge of (see \ref{fig:tdust}) ).
The structure of a PDR is governed by the intensity of the UV radiation field impinging onto the cloud surface (Go) in units of the ?. FUV flux (1.6 x107 ergs em? s7!). with GoxNU3Hn.“Lyy (2).. where y is the fraction luminosity over 6 eV. and L, is the luminosity of the star.
The structure of a PDR is governed by the intensity of the UV radiation field impinging onto the cloud surface $G_0$ ) in units of the \citet{ha68} FUV flux (1.6 $^{-3}$ ergs $^{-2}$ $^{-1}$ ), with $G_0\propto N_{\rm Lyc}^{-2/3}\ \ n_e^{4/3}\ \ L_{\star}\ \chi$ \citep{ti05}, , where $\chi$ is the fraction luminosity over 6 eV, and $L_{\star}$ is the luminosity of the star.
Adopting Nj, = 1.07 107? s! and L = 7.6» 107 Ls (2). y 2 Land considering n,= 75 — 154 em73 (see Sect.
Adopting $N_{\rm Ly}$ = $\times$ $^{48}$ $^{-1}$ and $L$ = 7.6 $\times$ $^4$ $L_{\odot}$ \citep{st03}, , $\chi$ = 1, and considering $n_e\simeq$ 75 – 154 3 (see Sect.
3.2). a range of Gy (0.5 - 1.5) x |0? is obtained.
3.2), a range of $G_0\simeq$ (0.5 - 1.5) $\times$ $^3$ is obtained.
The distribution of dust temperature in the PDR (rin is governed by the absorption of the stellar photons which are reemited by dust grains as IR photons.
The distribution of dust temperature in the PDR $T_d^{pdr}$ ) is governed by the absorption of the stellar photons which are reemited by dust grains as IR photons.
Following ?.. we can relate T with the visual absorption along the PDR (Αν) as.
Following \citet{ti05}, we can relate $T_d^{pdr}$ with the visual absorption along the PDR $A_{\rm v}$ ) as.
.. Considering both. the position of 33503 at the edge of clump A. and that the low value of visual absorption derived for the members of 117 (A, = 1.6 mag. ?)) is probably due to the interstellar absorption in the line of sight of the Hirregion. we Cal assume A,~ O for the surface of the PDR.
Considering both, the position of 3503 at the edge of clump A, and that the low value of visual absorption derived for the members of 17 $\bar{A}_{\rm v}$ = 1.6 mag, \citealt{pco10}) ) is probably due to the interstellar absorption in the line of sight of the region, we can assume $A_{\rm v}\sim$ 0 for the surface of the PDR.
Taking into account the range of Go and Eq. 14..
Taking into account the range of $G_0$ and Eq. \ref{g0},
we obtainK.. in accordance with the observed dust color temperature estimated for 33503K).
we obtain, in accordance with the observed dust color temperature estimated for 3503.
. This gives additional support to the existence of a PDR between and clump A. Figure IO displays a composite image of NGC3503 and its environs.
This gives additional support to the existence of a PDR between and clump A. Figure \ref{fig:champ-ir-halfa} displays a composite image of NGC3503 and its environs.
White and light blue contours show the radio continuum emission at 4800 MHz corresponding to NGC3503 and MBO. and the CO emission. respectively.
White and light blue contours show the radio continuum emission at 4800 MHz corresponding to NGC3503 and MBO, and the CO emission, respectively.
The color scale shows the emissior at 5 um (red) and 4.5 jm (green).
The color scale shows the emission at 8 $\mu$ m (red) and 4.5 $\mu$ m (green).
As described in Sect.
As described in Sect.
3.3 and 4.3. emission attributed to PAHs encircles the southern and western borders of the region. indicating the location of the PDR.
3.3 and 4.3, emission attributed to PAHs encircles the southern and western borders of the region, indicating the location of the PDR.
The position of NGC 3503 near the border of clump A and the existence of an electron density gradient along the symmetry axis of the region (with the higher electron densities close to the strongest CO emission) suggest that the tonised gas is being streamed away from the densest part of the molecular cloud.
The position of NGC 3503 near the border of clump A and the existence of an electron density gradient along the symmetry axis of the region (with the higher electron densities close to the strongest CO emission) suggest that the ionised gas is being streamed away from the densest part of the molecular cloud.
This is indicative that is a blister-type region that probably has undergone a champagne phase.
This is indicative that is a blister-type region \citep{i78} that probably has undergone a champagne phase.
The so-calledmodel (22?) proposes that an expanding Hirregion placed at the edge of a molecular cloud eventually reaches the border of the cloud and expands freely i1 the lower density surrounding gas. originating an extended Huregion. with a characteristic density distribution.
The so-called \citep{tt79,btt81,ttb82} proposes that an expanding region placed at the edge of a molecular cloud eventually reaches the border of the cloud and expands freely in the lower density surrounding gas, originating an extended region with a characteristic density distribution.
The Hüuregion becomes density bounded towards the lower density region. while it is 1onization bounded towards the molecular cloud.
The region becomes density bounded towards the lower density region, while it is ionization bounded towards the molecular cloud.
This scenario was formerly proposed by ? to explain the electron density gradient observed across NGC 3503.
This scenario was formerly proposed by \citet{c00} to explain the electron density gradient observed across NGC 3503.
The location of Pis 17 close to the brightest radio continuum region 1s consistent with à projection effect (?)..
The location of Pis 17 close to the brightest radio continuum region is consistent with a projection effect \citep{ytb83}.
In this scenario. Pis 17 originated NGC 3503. which reached the northeastern border of after 2x 10? yr.
In this scenario, Pis 17 originated NGC 3503, which reached the northeastern border of after $\times$ $^5$ yr.
This time represents à lower limit to the age of the Hitregion. since the inferred main-sequence life time of the main ionizing star is about (2)..
This time represents a lower limit to the age of the region, since the inferred main-sequence life time of the main ionizing star is about \citep{m98}.
The leakage of ionized gas and UV photons might have contributed to the formation of MBO. since its location (along the symmetry axis of )) and its lowdensity (about half of )) suggest that this feature may consist of tonizedgas which has scaped from after a time of 2x 10? yr.
The leakage of ionized gas and UV photons might have contributed to the formation of MBO, since its location (along the symmetry axis of ) and its lowdensity (about half of ) suggest that this feature may consist of ionizedgas which has scaped from after a time of $\times$ $^5$ yr.
The velocities of both the molecular and tonized gas are compatible with the champagne scenario.
The velocities of both the molecular and ionized gas are compatible with the champagne scenario.
The mean velocity
The mean velocity
CoRol-7 is an active Weewarl which was monitored photometrically for 5 months in 20072008 as part of the exoplanet programme of the ColtoT space mission (Baglin 2003).
CoRoT-7 is an active K-dwarf which was monitored photometrically for 5 months in 2007–2008 as part of the exoplanet programme of the CoRoT space mission \citep{Bag03}.
. Following the routine analysis of the data to search for. planetary transits.. Léger»etal.(2009hereafter.⋅LOO) . . . PN . ↓⋅⋖⊾↓≻∪↓⋅↿⋖⊾∠⇂∣⇂∐⊾∠⇂⋖⋅↿⋖⊾≼↛∣↓∪⊔⋡↓⊔≺∪∐∪↓−⋀⋡∖↓↓⋏↳≻⇂∐≼∙⊔↓⋅∖⇁⋖⊾⋡∪⇂⋖⊾≼↛↓↓↓≻⋡∖⋖⊾⋡∖. ∖∖⋰↓↓↥⋜↧∠⇂⋖⊾↓≻↿↓↥∩⇂⋅∪⊳∶∫≻⊔↓⊔↓⊔↓⋜↧⋅≟⋜⋯∠⇂⋜↧↓≻⋖⊾↓⋰↓⇜⊔↗∕↾∶∪⋅↖∖⋅↱≻≟∠∐⋡ superimposed on significant peak-to-peak) stellar variability.
Following the routine analysis of the data to search for planetary transits, \citet[][hereafter L09]{Leg09} reported the detection, in CoRoT-7's light curve, of eclipses with a depth of mmag and a period $P_b=0.854$ d, superimposed on significant peak-to-peak) stellar variability.
They also carried out. grouncl- photometric follow-up and obtained near-infrared spectra. which ruled out the majority of the alternative binary scenarios that could have given rise to the observed transits (grazing or diluted eclipsing svstems with a stellur. sub-stellar or giant planet. companion).
They also carried out ground-based photometric follow-up and obtained near-infrared spectra, which ruled out the majority of the alternative binary scenarios that could have given rise to the observed transits (grazing or diluted eclipsing systems with a stellar, sub-stellar or giant planet companion).
"They. therefore interpreted. the eclipses as most. likely to. be caused by aκ planetaryκdare pscompanion.ani dubbed:. 1οColtoT-Tb.τιτ witha a radiusparc] geἑ«tyop "Phe ∪⇂∫↘∕↾≓↓⋅↖∖⇁∪⋅−⋝∫⊓⊳↓∐∢≺⊔∩
They therefore interpreted the eclipses as most likely to be caused by a planetary companion, dubbed CoRoT-7b, with a radius of $R_b =1.8\pm0.2\, R_{\oplus}$.
⋟⊔↓↓≻≺⋯⋅∖↓⊔∆∎≟↓≺⊔∐≺↧↓∖∢↓⋯∐⋅∖aecanv] iz ⇁⋅ (RV) follow-up campaign. carried out with the LLARDS spectrograph. was reported in Quelozetal.(2009.hereafter Q09)..
The accompanying radial velocity (RV) follow-up campaign, carried out with the HARPS spectrograph, was reported in \citet[][hereafter Q09]{Que09}.
Phe RV signal of ColtoT-7 was dominated by strong ss.| peak-to-peak) activitv-induced variations.
The RV signal of CoRoT-7 was dominated by strong $^{-1}$ peak-to-peak) activity-induced variations.
Q09 nonetheless derived a racial velocity semi-amplitude of
Q09 nonetheless derived a radial velocity semi-amplitude of
Camzadvan&Penrose(2010) 6o. Wels Moss.Scott&Zibin(20411) IHajau(20010) Very recently" iua paper called “CCCpredicted loxc-viurdiiuice circles iu the CMD sky aud LCDI. Curzadvan&Penrose(2011) make a second attenipt at the same claim. this time anning to build their stations with a proper power spectrum.
\citet{gurzadyan:2010} $6\sigma$ \citet{wehus:2011}, \citet{moss:2011} \citet{hajian:2010} Very recently, in a paper called “CCC-predicted low-variance circles in the CMB sky and LCDM”, \citet{gurzadyan:2011a} make a second attempt at the same claim, this time aiming to build their simulations with a proper power spectrum.
Specifically. they claim that if the rancom simulation is built frou the "observed WALAP spectrum’. ic..
Specifically, they claim that if the random simulation is built from the “observed WMAP spectrum”, ie.,
the realization specific spectrum as directly measured by WALAP. the statistical sienficance of the rings is low. m agreement with the results of the three indepeudent reanalvses.
the realization specific spectrum as directly measured by WMAP, the statistical signficance of the rings is low, in agreement with the results of the three independent reanalyses.
However. if the sumuulatious are instead based on a theoretical (iiooth) ACDM spectrum. they claim that the rings are sieuificaut.
However, if the simulations are instead based on a theoretical (smooth) $\Lambda$ CDM spectrum, they claim that the rings are significant.
Their hypothesis is thus that the bumps aud wieeles in the WALAP spectruii frou cosmic variance carries extra information. leading to a greater probability of generating coherent rings (or vice versa. clepending on ones poiut-of-view).
Their hypothesis is thus that the bumps and wiggles in the WMAP spectrum from cosmic variance carries extra information, leading to a greater probability of generating coherent rings (or vice versa, depending on ones point-of-view).
Tere it is worth noting a few facts;
Here it is worth noting a few facts.
First. as clearly stated im cach of the three reanalysis papers. the siuulations used in cach case were du fact based on the best-fit ACDAL spectymn. not the realizatiou-specific WALAP spectrum.
First, as clearly stated in each of the three reanalysis papers, the simulations used in each case were in fact based on the best-fit $\Lambda$ CDM spectrum, not the realization-specific WMAP spectrum.
This is in) accordance with the eenerally accepted procedure for generatiug random CAIB simulation: usage of constrained spectruuui realization is a very special case. and would clearly warrant special justification.
This is in accordance with the generally accepted procedure for generating random CMB simulation; usage of constrained spectrum realization is a very special case, and would clearly warrant special justification.
This poiut alone shows that the updated claims by Carzadvan and Penrose are still wrone: One does of course find similar ringswith a ACDAL spectimm. and not only with the WALAP
This point alone shows that the updated claims by Gurzadyan and Penrose are still wrong: One does of course find similar ringswith a $\Lambda$ CDM spectrum, and not only with the WMAP
With an apparent CO luminosity ercater than that of the stronely lensed quasar APM 0827915255. the .=1135 quasar PSS 2322|1911 is the strongest CO emitter detected to date at redshifts larger than 3.5.
With an apparent CO luminosity greater than that of the strongly lensed quasar APM 08279+5255, the $z = 4.12$ quasar PSS 2322+1944 is the strongest CO emitter detected to date at redshifts larger than 3.5.
Asstuine uo eravitational magnification. we estimate a molecular gas mass of z2.5«JOHAL... and a far-intrarce luminosity of ~--2.1«1077E...
Assuming no gravitational magnification, we estimate a molecular gas mass of $\approx 2.5 \times 10^{11} \, \rm M_\odot$, and a far-infrared luminosity of $\rm \approx 2.7 \times 10^{13} \, L_{\odot}$.
The spectral energy distribution aud large Iuminositv sugeest that a massive starburst takes place iu PSS 2322|1911. which παν be related to the formation of the core o an elliptical ealaxy.
The spectral energy distribution and large luminosity suggest that a massive starburst takes place in PSS 2322+1944, which may be related to the formation of the core of an elliptical galaxy.
The exceptional brigl:ness of PSS 2322|19l niadkes it a good target for further oservations of oher CO transitions. in particular those from lower levels which will constrain the plivsical conditions of the buk of the molecular gas.
The exceptional brightness of PSS 2322+1944 makes it a good target for further observations of other CO transitions, in particular those from lower levels which will constrain the physical conditions of the bulk of the molecular gas.
Higher spatial resolution neasrelents are also needed to see whether the line or coutimain enissiou js extened. as it was seen for the radio aud optical enudssion (Carilli et al.
Higher spatial resolution measurements are also needed to see whether the line or continuum emission is extended, as it was seen for the radio and optical emission (Carilli et al.
20015: Djorgovski et al.
2001b; Djorgovski et al.,
oeim prep.).
in prep.).
The detection of CO in another strong (sub)mnillimeter contiuuuu hieh-: quasar confirms a frequent correlation between the 3 nun CO peak intensity aud he 1.3 mum conutiuuuu fux. with a typical ratio of about nity.
The detection of CO in another strong (sub)millimeter continuum $z$ quasar confirms a frequent correlation between the 3 mm CO peak intensity and the 1.3 mm continuum flux, with a typical ratio of about unity.
This relation shows that systematic searches for CO Cluission iu strong thermal dust coutiuuuni quasars are pronusine with current imstruneutalon. provided that the redshift is kuown with high enough accuracy.
This relation shows that systematic searches for CO emission in strong thermal dust continuum quasars are promising with current instrumentation, provided that the redshift is known with high enough accuracy.
Systematic (subjuullameter coutiuuuni strvevs of high redshift. radio-quiet quasars are therefore needed to fiud strong contimmiun sources towards which CO emission can be searched.
Systematic (sub)millimeter continuum surveys of high redshift, radio-quiet quasars are therefore needed to find strong continuum sources towards which CO emission can be searched.
Such studies promise to further our understanding of the physical and chemical properties of the most energetic sources in the early Universe.
Such studies promise to further our understanding of the physical and chemical properties of the most energetic sources in the early Universe.
Tnterferometric observations. especially with ALATA aud EVLA. will eventually be able to show the spatial distribution of the molecular eas aid its relation to the stars and ionized gas.
Interferometric observations, especially with ALMA and EVLA, will eventually be able to show the spatial distribution of the molecular gas and its relation to the stars and ionized gas.