source
stringlengths 1
2.05k
⌀ | target
stringlengths 1
11.7k
|
|---|---|
predictwcesplorethecorrelationbetwcen|a fEe| and age to show the diagnostic power of [a /Fe| as a stand-in for age. | In \\ref{s:predict} we explore the correlation between $\alpha$ /Fe] and age to show the diagnostic power of $\alpha$ /Fe] as a stand-in for age. |
Finally. in refsiconcl we sunuuanze our results aud conclusions. | Finally, in \\ref{s:concl} we summarize our results and conclusions. |
We analyze the results of an N body | SPI siuulation designed to mumic the quicscent formation and evolution of a Milkv Wayass ealaxy following the last major merger. | We analyze the results of an $N$ –body + SPH simulation designed to mimic the quiescent formation and evolution of a Milky Way–mass galaxy following the last major merger. |
The system is initialized as iu I&aufniaunetal.(2007) and ROSab ancl consists of a rotating. pressuresupported eas halo embedded in au NEW (Navarroctal.1997) dark matter halo. | The system is initialized as in \cite{Kaufmann2007} and R08ab and consists of a rotating, pressure–supported gas halo embedded in an NFW \citep{Navarro1997}
dark matter halo. |
This station was evolved for 10 Cyr using the parallel Α΄ body| SPIT code. GASOLINE (Wadsleyetal. 2001). | This simulation was evolved for 10 Gyr using the parallel $N$ $+$ SPH code, GASOLINE \citep{Wadsley2004}. |
.. As the simulation proceeds. the gas cools aud collapses to the ceuter of the halo. forming a thin disk from the insideout. | As the simulation proceeds, the gas cools and collapses to the center of the halo, forming a thin disk from the inside–out. |
Cas is continually infalling from the hot halo outo the disk for the duration of the simulation. | Gas is continually infalling from the hot halo onto the disk for the duration of the simulation. |
Star | Star |
Two Micron AME Sky Survey were extracted. via the Infrared Processing and AXnalvsis Center (PAC) WWW site. | Two Micron All Sky Survey were extracted via the Infrared Processing and Analysis Center (IPAC) WWW site. |
2MLASS has finished. uniformly scanning the entire sky in three near-infrared) bands. J. 11. and. Kes. using a pixel size of 27. | 2MASS has finished uniformly scanning the entire sky in three near-infrared bands, J, H, and $_S$, using a pixel size of 2”. |
2ALASS point-source photometry achieves a 10-0 (0.100 mag) detection at the following magnitude levels: ο) = 158. 1Η = 15.1. and Ix« = 14.3 for unconfusecl sources outside of the Galactic plane. | 2MASS point-source photometry achieves a $\sigma$ (0.109 mag) detection at the following magnitude levels: J = 15.8, H = 15.1, and $_S$ = 14.3 for unconfused sources outside of the Galactic plane. |
The second. incremental cata release contains data for four of our CIIVCS (bere are no data available for LUPASS J1712-64). | The second incremental data release contains data for four of our CHVCs (there are no data available for HIPASS J1712-64). |
A major advantage of using the 2\LASS archive for our search for stellar content is that we can casily obtain data covering a field of view which is well matched to he angular size ofa CLIVC. | A major advantage of using the 2MASS archive for our search for stellar content is that we can easily obtain data covering a field of view which is well matched to the angular size of a CHVC. |
To this end we extracted [rom he point source catalog all sources within a 1" racius of he centre of cach CLIYC (as well as for several companion ealaxies of the Milkv Way). | To this end we extracted from the point source catalog all sources within a $^o$ radius of the centre of each CHVC (as well as for several companion galaxies of the Milky Way). |
A further advantage of the PALASS data is that they allow us to investigate Calactic oreerouncl contamination. | A further advantage of the 2MASS data is that they allow us to investigate Galactic foreground contamination. |
We thus also extracted. data in comparison fields. at the same Galactic latitude. b. but at ongitudes of 1137. and 1-5". for cach cloud. (no data are available for the 5° field of LIVCO89-37-231). | We thus also extracted data in comparison fields, at the same Galactic latitude, b, but at longitudes of $^o$, and $^o$, for each cloud (no data are available for the $^o$ field of HVC039-37-231). |
The source count in each of these fields is around tenthousand. but with considerable variation. | The source count in each of these fields is around tenthousand, but with considerable variation. |
The latter is explained in part by the dillerences in area coverage within each of the 2" fields --Iustrated in Pies. | The latter is explained in part by the differences in area coverage within each of the $^o$ fields illustrated in Figs. |
6 7 (in addition to true variation cue o cüllerent. Galactic coordinates) | 6 7 (in addition to true variation due to different Galactic coordinates). |
In Figure 6. we display positional plots of the sources etected by 2ALASS. | In Figure 6, we display positional plots of the sources detected by 2MASS. |
Figure 7 shows results for olfset fields. | Figure 7 shows results for offset fields. |
There are no enhancements of stellar density visible toward 1e centres of the “ON” fields which could be interpreted as warf galaxies in the clouds. | There are no enhancements of stellar density visible toward the centres of the “ON" fields which could be interpreted as dwarf galaxies in the clouds. |
Phe “OPEL” fields exhibit a high gaellar density. showing that even at Galactic latitudes above Yo the Galactic foreground contamination is strong in the near infrared. | The “OFF" fields exhibit a high stellar density, showing that even at Galactic latitudes above $^o$, the Galactic foreground contamination is strong in the near infrared. |
The ON and OFF fields. are qualitatively similar. | The ON and OFF fields are qualitatively similar. |
| one-dimensional KS test on the [x-band. LEs agrees with this statement (although the probabilities diller larecly [rom case {ο case possibly due to small real variations with position over a few degrees in the Galaxy). | A one-dimensional KS test on the K-band LFs agrees with this statement (although the probabilities differ largely from case to case – possibly due to small real variations with position over a few degrees in the Galaxy). |
The distribution of sources on the ON CMDSs is concluded to be consistent with a population of Galactic foreground stars. | The distribution of sources on the ON CMDs is concluded to be consistent with a population of Galactic foreground stars. |
This leads us to favor the hypothesis that there are no associated stellar populations detected in these CIIVCS. | This leads us to favor the hypothesis that there are no associated stellar populations detected in these CHVCs. |
In Figure S. we show the J-Ixs. Ks} CMDs of the data. | In Figure 8, we show the $_S$, $_S$ ] CMDs of the data. |
We do not show CMDs of the OFF fields. because there is no obvious dillerence. between the CMDs of the ON and the OFF. leds. | We do not show CMDs of the OFF fields because there is no obvious difference between the CMDs of the ON and the OFF fieds. |
The same is true for other filter combinations. such as the J-H. HI]. or γιοι Ws] €MDs. | The same is true for other filter combinations, such as the [J-H, H], or $_S$, $_S$ ] CMDs. |
We overplotted Girardi et al. ( | We overplotted Girardi et al. ( |
2000) isochrones onto one of the J-Ixs. Ks] €CMDs. | 2000) isochrones onto one of the $_S$, $_S$ ] CMDs. |
At distances of around. 150 kpe (as shown in Fig. | At distances of around 150 kpc (as shown in Fig. |
SN). we can expect to detect the full range of red stellar populations. supergiants. AGB stars and also. stars along the RGB. | 8), we can expect to detect the full range of red stellar populations, supergiants, AGB stars and also, stars along the RGB. |
Only for distances of less than about 300 Ixpe do the data include the TICD. | Only for distances of less than about 300 Kpc do the data include the TRGB. |
For a distance of 1 Alpe. we could at best expect to detect red supergiants in associated ealaxies with these data. | For a distance of 1 Mpc, we could at best expect to detect red supergiants in associated galaxies with these data. |
This limits the tests we can perfom with the 2\LASS data. | This limits the tests we can perfom with the 2MASS data. |
On the other hand. as shown by Fig. | On the other hand, as shown by Fig. |
S. the 2\LASS data complement the optical data in ruling out the presence ofa voung stellar population. | 8, the 2MASS data complement the optical data in ruling out the presence of a young stellar population. |
‘They do so even in the presence of a small amount of internal dust. since absorption is much smaller in the near-Lt than in the optical. | They do so even in the presence of a small amount of internal dust, since absorption is much smaller in the near-IR than in the optical. |
The 2ALASS data are a powerful. tool to separate a potential very voung stellar. population in ΕΝΟΣ from Galactic foreground stars. | The 2MASS data are a powerful tool to separate a potential very young stellar population in HVCs from Galactic foreground stars. |
Notice how the LO Myr isochrone of Fig. | Notice how the 10 Myr isochrone of Fig. |
S runs through a part of the CMD where LEVC'039-37-231 does not exhibit any stars. | 8 runs through a part of the CMD where HVC039-37-231 does not exhibit any stars. |
The 2ALASS data are actually sensitive to 10-Myr-old AIS stars for clistances of up to 125 Ixpc. and for 10-Myr-old. BSC: stars for clistances of up to 500 Ίνρο. | The 2MASS data are actually sensitive to 10-Myr-old MS stars for distances of up to 125 Kpc, and for 10-Myr-old BSG stars for distances of up to 500 Kpc. |
The lack of stars with colours ]x« «0.2 demonstrates that we do not detect a voung stellar component in the CLIIVCSs out to large distances. | The lack of stars with colours $_S$$<$ 0.2 demonstrates that we do not detect a young stellar component in the CHVCs out to large distances. |
The 2NLASS data are also uniquely sensitive to voung and intermediate-age ACD stars for distances of less than about 300 Ixpc. | The 2MASS data are also uniquely sensitive to young and intermediate-age AGB stars for distances of less than about 300 Kpc. |
See how old isochrones in Fig. | See how old isochrones in Fig. |
S stick out of the data distribution. | 8 stick out of the data distribution. |
They terminate at the first thermal pulse and so. do not extend as far red in colour as the full range of AGB stars seen. e.g. in the LMC and SAIC (see below). | They terminate at the first thermal pulse and so, do not extend as far red in colour as the full range of AGB stars seen, e.g., in the LMC and SMC (see below). |
There are no stars with Ixs« 14 and J-Ix 571. where we would expect to see the AGB component of CLIVCS for distances less than about 300 Ixpe. | There are no stars with $_S$$<$ 14 and $_S$$>$ 1, where we would expect to see the AGB component of CHVCs for distances less than about 300 Kpc. |
The cistribution of sources in this colour and magnitude range is instead. Cully consistent with Galactic foreground. only. | The distribution of sources in this colour and magnitude range is instead fully consistent with Galactic foreground, only. |
that the magnetic Revnolds uuuber is probably very (<< 1) for UCDs with convective velocities below 100 1. | that the magnetic Reynolds number is probably very $<1$ ) for UCDs with convective velocities below 100 $^{-1}$. |
This ueutralitv of UCD photospicres cun be reconclled with the relatively Ligh electro1 colui deusities mferred by Berger (2Q02)) on the assmuptiona that the τας10 Cluission is primarily duc to a high density of electrous. | This neutrality of UCD photospheres can be reconciled with the relatively high electron column densities inferred by Berger \cite{berger02}) ) on the assumption that the radio emission is primarily due to a high density of electrons. |
Iu their own Lhand monitorug of 15 L chwarts. Cehno ct ((2002)) found seven to be variable. and concluded ou the basis of t1C nettrality of L dwarts that the variability was not magjetic 11rorein. | In their own I-band monitoring of 18 L dwarfs, Gelino et \cite{gelino02}) ) found seven to be variable, and concluded on the basis of the neutrality of L dwarfs that the variability was not magnetic in origin. |
Further. noct ((20 H3) detected photometric variability in t1ο feld. M9. dwarf 0911. which eenuerallv shows very weak. nuvenetic activiv. although an Πα flare has been observe froi this ob.ject (Reid e citereid99)). | Further, n et \cite{martin01}) ) detected photometric variability in the field M9 dwarf $-$ 0214, which generally shows very weak magnetic activity, although an $\alpha$ flare has been observed from this object (Reid et \\cite{reid99}) ). |
This returns Us to the behaviour of dust. | This returns us to the behaviour of dust. |
m a cool static atnosphere. dust graius wi] form. grow aud eravitationally settle below the ploosphere creating a clust-clearec|l photosphere depleted im those elements locked into he erains. | In a cool static atmosphere, dust grains will form, grow and gravitationally settle below the photosphere creating a dust-cleared photosphere depleted in those elements locked into the grains. |
By coutrast. in a. dynamic atmosphere. cconvection will provide a bouvaney acting agalust preci]tation. and deep convection av recycle precipitated elements back iuto the visible atinosphere. thus retainiug a dusty couposition. | By contrast, in a dynamic atmosphere, convection will provide a bouyancy acting against precipitation, and deep convection may recycle precipitated elements back into the visible atmosphere, thus retaining a dusty composition. |
First attempts to consider the relative cfficicney of dust settling and convective recveling — aud hence the verticaddistiibution of dust eraius iu the plotosplere have been nude by Tsuji (2001)) and Ackernan Marev (2001)). | First attempts to consider the relative efficiency of dust settling and convective recycling – and hence the distribution of dust grains in the photosphere – have been made by Tsuji \cite{tsuji01}) ) and Ackerman Marley \cite{ackerman01}) ). |
A exadual rausition from a dusty to a dus-cleared atmospliere is xedieted to occur with decreasing effective temperature. | A gradual transition from a dusty to a dust-cleared atmosphere is predicted to occur with decreasing effective temperature. |
Dust can be considered to be confined to a thin laver. he depth (pressure) of the base of which is determined w the coudeusation temperature of eraius. | Dust can be considered to be confined to a thin layer, the depth (pressure) of the base of which is determined by the condensation temperature of grains. |
Condcusation can occur throughout he atinosphere above this base with iucreasiue ficiency at higher altitudes (due to lower eniperatures). although with decreasing coutributiou to he opacity οἱ1 account of the decreasing deusitv. | Condensation can occur throughout the atmosphere above this base with increasing efficiency at higher altitudes (due to lower temperatures), although with decreasing contribution to the opacity on account of the decreasing density. |
A limit on the verticeUo extent of this laver may be set by the erowth of erains above some critical size. at which point eyavity OVCLCOmes turbulent support aud these erains are precipitated «mt iuto deeper lavers of the atmosphere. | A limit on the vertical extent of this layer may be set by the growth of grains above some critical size, at which point gravity overcomes turbulent support and these grains are precipitated out into deeper layers of the atmosphere. |
As the effective temperature decreases. tlhe base of this dust liver moves to deeper parts of the amosphere. where the inteerated eas opacity (as seen from outside the photosphere} is dnereased. | As the effective temperature decreases, the base of this dust layer moves to deeper parts of the atmosphere, where the integrated gas opacity (as seen from outside the photosphere) is increased. |
Ποσο the cust laver becomes less visible wih the result that the spectrum increasingly represents a ¢ust-cleared atiiosphliere. | Hence the dust layer becomes less visible with the result that the spectrum increasingly represents a dust-cleared atmosphere. |
Such a mechanisin may explain the switch from red to blue infrared colours for the transition from mud L chwarts to T dwarts. | Such a mechanism may explain the switch from red to blue infrared colours for the transition from mid L dwarfs to T dwarfs. |
Neither tre model of Tsuji (2001)) nor that of Ackerman Marley (20013) addresses the possibility ofhorizontal Inhomoecneities or dust grain dynamics which would be required to produce variability in the unresolved disk (but see IIelliug ct citehelling01)). | Neither the model of Tsuji \cite{tsuji01}) ) nor that of Ackerman Marley \cite{ackerman01}) ) addresses the possibility of inhomogeneities or dust grain dynamics which would be required to produce variability in the unresolved disk (but see Helling et \\cite{helling01}) ). |
Iu a dusty or dust-cleared atiuosphiere. these inhonogencitics cotud be regions of cuhanced dust formation and dust opacitv. perhaps due to a localized deep couvective column bringing dust forming material up from fje deeper. opaque lavers of the atmosphere. | In a dusty or dust-cleared atmosphere, these inhomogeneities could be regions of enhanced dust formation and dust opacity, perhaps due to a localized deep convective column bringing dust forming material up from the deeper, opaque layers of the atmosphere. |
Alternatively. im a dusty atinosphliere. dust formation may be slow in the material |ought up by deep convection. thus creatiie a short-liv«L dust-free cloud. | Alternatively, in a dusty atmosphere, dust formation may be slow in the material brought up by deep convection, thus creating a short-lived dust-free cloud. |
lu the preseut paper. I report the results of au observational prograin to investigate further the physical cause of variaality in CCDs. | In the present paper, I report the results of an observational program to investigate further the physical cause of variability in UCDs. |
Such an investigation is naturally rather speculative given how little we known of tiiie-depeudenu ΕΕric processes in UCDs. | Such an investigation is naturally rather speculative given how little we known of time-dependent atmospheric processes in UCDs. |
Iu light of this. I decided. to. specrophotometrically monitor a UCD over a wide wavelength range. | In light of this, I decided to spectrophotometrically monitor a UCD over a wide wavelength range. |
The near mfrared (NIR) region nucrou)) was chosen over the optical uucron)) 1OCAse UCDs are significantly brighter there. | The near infrared (NIR) region ) was chosen over the optical ) because UCDs are significantly brighter there. |
At the time of targe selectiou (July 1999). the ouly known photoiotricalv. variable UCDs were the LL5 dwarf (Dailer-Jones Aluudt 19 903) and tιο MO. dwarf LP911-20. (Tinney Tolley 1999)). | At the time of target selection (July 1999), the only known photometrically variable UCDs were the L1.5 dwarf (Bailer-Jones Mundt \cite{bjm99}) ) and the M9 dwarf LP944-20 (Tinney Tolley \cite{tinney99}) ). |
The former was selected because (1) we intended to 1iouitor1 agal vin the Ehand aud (2) it has a nearby bright reference star which ca1i be used to obtain spectrophotomerv. | The former was selected because (1) we intended to monitor it again in the I-band and (2) it has a nearby bright reference star which can be used to obtain spectrophotometry. |
Due to rapid chiuges in sky trausnussion a1. brighness in f1ο NIR. it was felt that spectrophotomery frou regular calibration against standards was not viable. | Due to rapid changes in sky transmission and brightness in the NIR, it was felt that spectrophotometry from regular calibration against standards was not viable. |
Iistead. spectroplotometry is done relative fo a secoli| star in the same slit. on the assunption tiat this reference star is photometrically stable to some required kvO ou the timescale of iuterest. | Instead, spectrophotometry is done relative to a second star in the same slit, on the assumption that this reference star is photometrically stable to some required level on the timescale of interest. |
This reference star Gvhich is not prescutly iun NED or SIMBAD an is saturated in the data of BAIN) has designation231613.. and has D.R.J.II aud nunaegnitudes of 11.50. lL10. 13.57. 13.28 and 13.15 respectively. as taken frou he 2MASS second incremental release catalogue. | This reference star (which is not presently in NED or SIMBAD and is saturated in the data of BJM) has designation, and has B,R,J,H and magnitudes of 14.80, 14.10, 13.57, 13.28 and 13.18 respectively, as taken from the 2MASS second incremental release catalogue. |
These are lost consistent with an Tuarecened or slightly reddened iiüd- or Iate-tv)o E dwart. | These are most consistent with an unreddened or slightly reddened mid- or late-type F dwarf. |
The €alac‘tic latitude of the field is /=226° b=Th inplviie tiat it is probably an older thick disk «x halo star at skpe. rather than a very voung poteutialv variable star or pusating supoereiaut. ( | The Galactic latitude of the field is $l=226^{\circ}$, $b=75^{\circ}$, implying that it is probably an older thick disk or halo star at kpc, rather than a very young potentially variable star or pulsating supergiant. ( |
hereafter 2\TL115) isan L1.5 dwar: discovered by 2NTASS with LJ and ΠΠdes of 18.6. 15:37. 1152 and 13.92 respectively (Iirkpatiick et rick909:: the | hereafter 2M1145) isan L1.5 dwarf discovered by 2MASS with I,J,H and magnitudes of 18.6, 15.37, 14.52 and 13.92 respectively (Kirkpatrick et \\cite{kirkpatrick99}; ; the |
angle &. which leads to a longer arrival time due to a longer light distance (eq. | angle $\theta$, which leads to a longer arrival time due to a longer light distance (eq. [ |
1}. | 1]). |
Obviously. one can tell from Figure 4 that the visible softening emerges at later Gime when the steep decay (x/ 7) in the light curves shows up. | Obviously, one can tell from Figure 4 that the visible softening emerges at later time when the steep decay $\propto t^{-2}$ ) in the light curves shows up. |
This corresponds to a delaved. time of /;&Ρο~3x10!s(e/1keV)?(a/0.1jmi) ?CDu,/100pc). where f is the Planck constant. and A. €. and à are the equivalent average photon wavelength. energy. and dust radius. respectively. | This corresponds to a delayed time of $t_d\simeq (1+z_d)D_d D_{ds}\bar{\lambda}^2/(32
\pi c D_s \bar{a}^2)\simeq 3\times 10^4s(\bar{\epsilon}/1{\rm
keV})^{-2}(\bar{a}/0.1 \mu{\rm m })^{-2}(D_{ds}/100 {\rm pc})$ , where $h$ is the Planck constant, and $\bar{\lambda}$, $\bar{\epsilon}$, and $\bar{a}$ are the equivalent average photon wavelength, energy, and dust radius, respectively. |
Above. we revisit the X-ray seattering olf dust grains at CRB stages. | Above, we revisit the X-ray scattering off dust grains at GRB stages. |
Now we apply these results to observational data and suggest that some of the X-ray afterglows detected so [ar mav be alternatively explained as the emission [rom X-ray echoes. ie.. dust-scatteringdriven alterglows. | Now we apply these results to observational data and suggest that some of the X-ray afterglows detected so far may be alternatively explained as the emission from X-ray echoes, i.e., dust-scattering–driven afterglows. |
1. | 1. |
A shallow decay followed by a “normal” decay. ancl a further steepening is suggested by Zhang et al. ( | A shallow decay followed by a “normal" decay and a further steepening is suggested by Zhang et al. ( |
2006) to be characteristic of almost all the ο) GRBs. ( | 2006) to be characteristic of almost all the $Swift$ GRBs. ( |
1) In general. to account for shallow decay. a continuous activity of the GRB progenitor is expected (Dai&LuMészáros.2001:Dai2004) or a power law distribution of the Lorentz factors in the ejecta is assumed (Rees&Mésziros1998:SariMészáros2000). | 1) In general, to account for shallow decay, a continuous activity of the GRB progenitor is expected \citep{dl98,zm01,d04} or a power law distribution of the Lorentz factors in the ejecta is assumed \citep{rm98,sm00}. |
. Alternatively. we propose that this feature can be attributed to the X-ray echo emission al early limes. ( | Alternatively, we propose that this feature can be attributed to the X-ray echo emission at early times. ( |
2) To account for the steep decay alter (he “normal” decay. the relativistic jet effect has been suggested (Rhoads1999;Sari.Piran.&IHlalpern.1999). | 2) To account for the steep decay after the “normal" decay, the relativistic jet effect has been suggested \citep{r99,s99}. |
. Alternatively. this feature can be explained as (he X-ray echo emission al late times. | Alternatively, this feature can be explained as the X-ray echo emission at late times. |
To summarize. the features with a shallow decay followed by a “normal” decay. and a further steepening are consistent. wilh the X-ray echo emission presented above. e. &.. as shown in Figure 3. | To summarize, the features with a shallow decay followed by a “normal" decay and a further steepening are consistent with the X-ray echo emission presented above, e. g., as shown in Figure 3. |
lere. we apply equation (13) to two recently detected. GRBs. 060813. and 060814. in Figure 5. where 0c and E,~200 keV are assumed. | Here, we apply equation (13) to two recently detected GRBs, 060813 and 060814, in Figure 5, where $\delta\simeq 0$ and $E_p\simeq 200$ keV are assumed. |
The consequent parameters are aq290.54 and Dyas210 pe for GRB 060813 and α£20.25jm and Dy,230 pe for GRB 060814. | The consequent parameters are $a_+\simeq
0.5\,\mu{\rm m}$ and $D_{ds}\simeq 10$ pc for GRB 060813 and $a_+\simeq 0.25\,\mu{\rm m}$ and $D_{ds}\simeq 30$ pc for GRB 060814. |
The other parameters. ¢£20.025jum. q224. and 5&2. ave the same for (he two GRBs. | The other parameters, $a_-\simeq 0.025\,\mu{\rm m}$, $q\simeq 4$, and $s\simeq 2$, are the same for the two GRBs. |
Obviously. a shallow decay is common in early X-ray afterglows. | Obviously, a shallow decay is common in early X-ray afterglows. |
This favors the cust-scattering scenario. which predicts a shallow decay at an early tme. when (he scattering angle is smaller (see also eq. [ | This favors the dust-scattering scenario, which predicts a shallow decay at an early time, when the scattering angle is smaller (see also eq. [ |
Subsets and Splits
No community queries yet
The top public SQL queries from the community will appear here once available.