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We find 27 point sources above 3 0 (~2 mJ) in the APEX-SZ maps using the approach outlined in refSUDSEC:psestinate.. | We find 27 point sources above 3 $\sigma$ $\sim$ 2 mJy) in the APEX-SZ maps using the approach outlined in \\ref{SUBSEC:psestimate}. |
Eight of these sources are within 1/of à NVSS source aud are likely radio sources. | Eight of these sources are within $^\prime$ of a NVSS source and are likely radio sources. |
We expect four false detections based on Cassia statistics and the number of beamrsized pixels iu the APEN-SZ imap. | We expect four false detections based on Gaussian statistics and the number of beam-sized pixels in the APEX-SZ map. |
The remaining sources are tentativelv identified as dusty galaxies. | The remaining sources are tentatively identified as dusty galaxies. |
We cun compare the observed nunber counts in the APENX-SZ maps with other experiments at 150 GIIz. however most previous experiments were tarecting larger angular scales aud are relatively iuseusitive to dini point sources; | We can compare the observed number counts in the APEX-SZ maps with other experiments at 150 GHz, however most previous experiments were targeting larger angular scales and are relatively insensitive to dim point sources. |
QUaD (?) and ACBAR (?) both report —0.1 radio sources per square degree with a flux detection threshold of may tens of indy. | QUaD \citep{friedman2009} and ACBAR \citep{reichardt2008} both report $\sim$ 0.1 radio sources per square degree with a flux detection threshold of many tens of mJy. |
The deepest previously published map at 150 CIIz is from Bolocai (2). which reports no sources above LO mJy in a 1 deg? patch. | The deepest previously published map at 150 GHz is from Bolocam \citep{sayers09} which reports no sources above 10 mJy in a 1 $^2$ patch. |
As dN(2S)/dS is expected to fall steeply above 1 12Jy for dusty ealaxies. the scarcity of detected sources in these maps is nof particularly surprising. | As $>$ S)/dS is expected to fall steeply above 1 mJy for dusty galaxies, the scarcity of detected sources in these maps is not particularly surprising. |
The BLAST source catalogue (1) of 351 sources detected at 250. 350 or 500 μπι allows a more interesting cross-colparison. | The BLAST source catalogue \citep{dye2009} of 351 sources detected at 250, 350 or 500 $\mu$ m allows a more interesting cross-comparison. |
The BLAST catalogue has 291 sources per square degree in the deep coverage region and 15 sources per square degree in the shallow coverage regiou. | The BLAST catalogue has 294 sources per square degree in the deep coverage region and 15 sources per square degree in the shallow coverage region. |
At 500 jou. the detection threshold of the BLAST catalogue is 30 µι]ν and 100 indy respectively. | At 500 $\mu$ m, the detection threshold of the BLAST catalogue is 30 mJy and 100 mJy respectively. |
For the best-fit effective spectral iudex of a=2.61 derived earlier. this correspouds to a source detection threshold at 150 Ον of 0.5 aud 2.6 mJy respectively. | For the best-fit effective spectral index of $\alpha=2.64$ derived earlier, this corresponds to a source detection threshold at 150 GHz of 0.8 and 2.6 mJy respectively. |
These two detection thresholds bracket the average APEN-SZ 36 detection threshold of 2 παν. aud the observed APEN-SZ nou-racdio source unuber density of 19 sources/deg? falls between these two source densities as we would expect. | These two detection thresholds bracket the average APEX-SZ $\,\sigma$ detection threshold of 2 mJy, and the observed APEX-SZ non-radio source number density of 19 $^2$ falls between these two source densities as we would expect. |
The source uunber counts in the APEN-SZ maps appear cousisteut with the wuubers expected for dusty galaxies. | The source number counts in the APEX-SZ maps appear consistent with the numbers expected for dusty galaxies. |
Observations with the APEN-SZ instrument have beeu used to constrain the power m excess of the primary CXMB temperature aulsotropies at 150 CGIIz. | Observations with the APEX-SZ instrument have been used to constrain the power in excess of the primary CMB temperature anisotropies at $150\,$ GHz. |
This power is expected to be dominated by cussion from sub-una bright. dusty galaxies and the APEN-SZ baud powers are cousistent with this hvpothesis. | This power is expected to be dominated by emission from sub-mm bright, dusty galaxies and the APEX-SZ band powers are consistent with this hypothesis. |
We find excelleu agreement between the point source power iu the APEX-SZ maps aud model predictions based ou observations a other frequencics. | We find excellent agreement between the point source power in the APEX-SZ maps and model predictions based on observations at other frequencies. |
We estimate that the fiux of these sub-unm bright galaxies scales with frequency as S,~778 * ColNparing the power measured by BLAST at 600 CGIIz to the best-fit point source power in the APEX-SZ maps at 150 GIIz. | We estimate that the flux of these sub-mm bright galaxies scales with frequency as $S_\nu \sim \nu^{2.64}$ by comparing the power measured by BLAST at 600 GHz to the best-fit point source power in the APEX-SZ maps at 150 GHz. |
Determining the contribution of hese foreground sources not only constrains models for he population of dusty galaxies. but is important for annus current aud future observations of secondary ΑΠΟ anisotropies at these waveleneths. | Determining the contribution of these foreground sources not only constrains models for the population of dusty galaxies, but is important for planning current and future observations of secondary CMB anisotropies at these wavelengths. |
We also place upper limits on c4 from fits to he amplitude of the SZE power spectrum while nareinalizinge over a Poisson point source coutribution. | We also place upper limits on $\sigma_8$ from fits to the amplitude of the SZE power spectrum while marginalizing over a Poisson point source contribution. |
We assume a template for the SZE power spectim derived from simulations by ? with the amplitude of the SZE power spectrum scaling as og. | We assume a template for the SZE power spectrum derived from simulations by \cite{shaw2009} with the amplitude of the SZE power spectrum scaling as $\sigma_8^7$ . |
We find an upper luit of ex<L.18 at confidence. | We find an upper limit of $\sigma_8< 1.18$ at confidence. |
This result is similar to the constraints from the CBI aud BIMA interferometers operating at 30 GIIz. | This result is similar to the constraints from the CBI and BIMA interferometers operating at $30\,$ GHz. |
The Bits frou SZA. QUaD. or ACBAR would likely be slightly lower. but they did not express their results iu terms of upper limits ou oy. | The limits from SZA, QUaD, or ACBAR would likely be slightly lower, but they did not express their results in terms of upper limits on $\sigma_8$. |
At these frequeucies aud angular scales. the previous best luit comes frou ?.. who used observations with the Bolocai iustruieut to coustrain ey«1.57 at 90% confidence. | At these frequencies and angular scales, the previous best limit comes from \citet{sayers09}, , who used observations with the Bolocam instrument to constrain $\sigma_8<1.57$ at $90\%$ confidence. |
A third of the APEN-SZ instrument was recentlv uperaded to more sensitive detectors with iuproved optical efficicucies. | A third of the APEX-SZ instrument was recently upgraded to more sensitive detectors with improved optical efficiencies. |
Iu the next vear. the reminderof the focal plane will be upgraded resulting in siguificaut | In the next year, the remainderof the focal plane will be upgraded resulting in significant |
population of clectrous with power-law index p as ys”. | population of electrons with power-law index $p$ as $n_0\gam^{-p}$. |
The total wuuber of relativistic electrons in one blob is The fraction of the relativistic electrons to the total iuuber of the initial blob is about «ΤΟgn= for p>2. where ©»τμ=£/0.01 and 5,44,=50. | The total number of relativistic electrons in one blob is The fraction of the relativistic electrons to the total number of the initial blob is about $\xi k\tss/\gmin m_ec^2=0.012\xi_{-2}$ for $p>2$, where $\xi_{-2}=\xi/0.01$ and $\gmin=50$. |
This stronely προς that the αμα electrons may originate from the present mechanism which may be a proposing nechanisuni responsible for the acceleration of relativistic olectrous in some of radio-loud quasars. | This strongly implies that the radiating electrons may originate from the present mechanism, which may be a proposing mechanism responsible for the acceleration of relativistic electrons in some of radio-loud quasars. |
It is expected the nouthermal emission spectra and light curves should be similar to some properties predicted by Li I&usunose (2000) ancl I&usunose et al. ( | It is expected the nonthermal emission spectrum and light curves should be similar to some properties predicted by Li Kusunose (2000) and Kusunose et al. ( |
2000). | 2000). |
It is thus inevitable for the ejected blob that the lugh-temperature drops due to the strong interaction between the blob aud its surroundings. aud as a natural consequence there is a eroup of clectrous to be accelerated to relativistic eucrev responsible for the coutimmim aud sole recombination lines from the cooled blob | It is thus inevitable for the ejected blob that the high-temperature drops due to the strong interaction between the blob and its surroundings, and as a natural consequence there is a group of electrons to be accelerated to relativistic energy responsible for the continuum and some recombination lines from the cooled blob. |
It has been generally accepted that accretion onto super massive black holes leads to the release of gravitational οποιον in active galactic nuclei (Rees 1981). | It has been generally accepted that accretion onto super massive black holes leads to the release of gravitational energy in active galactic nuclei (Rees 1984). |
However. the status of the accretion disk im differeut kinds of ACNs remains uncertain. | However, the status of the accretion disk in different kinds of AGNs remains uncertain. |
Iou-supported tori may power the central cneiue iu radio-loud quasars (Rees et al. | Ion-supported tori may power the central engine in radio-loud quasars (Rees et al. |
1982). | 1982). |
A famous low luminosity ACN NCC 1258 is cenerally thought as representative of ADAFs (Camunie et al. | A famous low luminosity AGN NGC 4258 is generally thought as representative of ADAFs (Gammie et al. |
1999). | 1999). |
However. receut observatious of bv show the origination is not from an accretion disk (Reynolds ct al. | However, recent observations of by show the origination is not from an accretion disk (Reynolds et al. |
Ww00). | 2000). |
Yaqoob et al. ( | Yaqoob et al. ( |
1999) detected a highly Dopplerbhic-shifted Ik-eiissiou line iu PISS 2119306. | 1999) detected a highly Doppler blue-shifted K-emission line in PKS 2149–306. |
We thus apply our model to the two objects. | We thus apply our model to the two objects. |
4255: The ass the central black hole is well determiued tobe sovationAL,or«10AZ, by. Mivoshi et al. ( | The mass of the central black hole is well determined to be $\mbh=3.6\times 10^7\sunm$ by Miyoshi et al. ( |
1995). | 1995). |
Radio ol set the transition radius frou the standard disk to the ADAF to be 10072, (Herrustein et al. | Radio observation set the transition radius from the standard disk to the ADAF to be $R_g$ (Herrnstein et al. |
1999). and the accretion rate is ~LO«10.PMg (Camuunie et al. | 1999), and the accretion rate is $\sim 1.0\times 10^{-3}\dot{M}_{\rm Edd}$ (Gammie et al. |
1999). | 1999). |
Taking the typical value of a=0.) we have T4LT& 10K and s4=7.2«Loan 7. if the ejection takes place at LOR,. where the viscous heating rate is lighest. | Taking the typical value of $\alpha=0.1$, we have $T_1=4.7\times 10^{10}$ K and $n_1=7.2\times 10^{10}$ $^{-3}$, if the ejection takes place at $R_g$, where the viscous heating rate is highest. |
The initial dimension of the ejected blob is taken to be Ry=108,104! cm. | The initial dimension of the ejected blob is taken to be $R_0=10R_g=10^{14}$ cm. |
The additional componcut with huninostv £4=2.0«10Ü cres/s idu N-ray shows that the teuuous plasma is of temperature 0.5 keV (Revnolds et al. | The additional component with luminosity $L_X^A=2.0\times 10^{40}$ ergs/s in X-ray shows that the tenuous plasma is of temperature 0.5 keV (Reynolds et al. |
2000). | 2000). |
This sets constraints on the density of the environment iu the vicinity of the uucleus via the Thomson scattering depth Ty=Oy,Nef. where σι, is the Thomson scattering cross section and f is the dimension of its surroundings. | This sets constraints on the density of the environment in the vicinity of the nucleus via the Thomson scattering depth $\tau_{_{\rm Th}} = \st n_2 \ell$, where $\st$ is the Thomson scattering cross section and $\ell$ is the dimension of its surroundings. |
Using the N-rav. luminosity of the additional componcut contributed. from. the teimous plasma L4=απ1mAn3T,yal/2 (A=3.1s10 25, we have the umuber density of the surroundings to be ny=TOy | Using the X-ray luminosity of the additional component contributed from the tenuous plasma $L_X^A=\frac{4}{3}\pi\ell^3 \Lambda n_2^2T_e^{1/2}$ $\Lambda=3.4\times 10^{-27}$ ), we have the number density of the surroundings to be $n_2=10^8(\tau_{_{\rm Th}}/0.1)^3$ $^{-3}$. |
From equation (1) we have the Mach munuber Moο=97. | From equation (4) we have the Mach number ${\cal M} = 97$. |
The timescale of cooling duc to expansion is then given bv τ2.36« 1078. which is much shorter than that of free cooling. | The timescale of cooling due to expansion is then given by $\tau=2.36\times 10^5$ s, which is much shorter than that of free-free cooling. |
The expanded radius of the blob is cu. | The expanded radius of the blob is cm. |
The temperature will drop from L7«1019. to T=Tj£M?x5.0«08h. Dining the cooling sole recombination lines will be produced (Ravinoud Sinith 1977). such as FeNNVIAL7SA.. FoNNVAI.85À.. FOXNVALAGA.. audRR line OVITTALS.97. aud silicou Si NIVAG.ISÁ.. ete. | The temperature will drop from $4.7\times 10^{10}$ K to $T=T_1/{\cal M}^2\approx 5.0\times 10^6$ K. During the cooling some recombination lines will be produced (Raymond Smith 1977), such as $\lambda1.78$, $\lambda1.85$ , $\lambda1.86$ , and oxygen line $\lambda18.97$, and silicon Si $\lambda 6.18$, etc. |
mIf the blob moves with Doppler factor of10 (Ganuuie et al. | If the blob moves with Doppler factor of10 (Gammie et al. |
we expect to observe the highly Doppler bluc-shifted line at GLPyy keV. where D=LODiy is the Doppler factor. | 1999), we expect to observe the highly Doppler blue-shifted line at $\cd_{10}$ keV, where $\cd=10\cd_{10}$ is the Doppler factor. |
Such lines should be detected by future observations ofINTEGRAL. | Such lines should be detected by future observations of. |
306: The lighly Doppler shifted iron EK-cussion line has been detected by in this hieh redshift (222.315) radio-loud quasar (Yaqoob et al. | The highly Doppler shifted iron K-emission line has been detected by in this high redshift $z$ =2.345) radio-loud quasar (Yaqoob et al. |
1999). although the curent data does not allow to determine its "uenbiguous profile. | 1999), although the current data does not allow to determine its unambiguous profile. |
We attempt to apply our prescut uodel to this source. | We attempt to apply our present model to this source. |
The central mass can be obtained roni the full-width-at-half-1naxiununmni CEWIIM) and the ununmositv of emission line CIV (Peterson 1998). | The central mass can be obtained from the full-width-at-half-maximum (FWHM) and the luminosity of emission line CIV (Peterson 1998). |
With the neasurements of Ον=6100kim/s (Wilkes 1986). aud L(CTV)=1.2xs10 eres (Wilkes et al. | With the measurements of $v_{_{\rm FWHM}}=6400$ km/s (Wilkes 1986), and $L({\rm CIV})=1.2\times 10^{46}$ erg/s (Wilkes et al. |
1983) (which we neasured from the spectrum). we have the mass of the central black hole. M=3.1«109AZ... which corresponds Eddinston huninositv =L3«10!ere/s. If we ollow the mean spectrum L,,,of radio-loud quasars (Elvis et al. | 1983) (which we measured from the spectrum), we have the mass of the central black hole, $\mbh=3.4\times 10^9\sunm$, which corresponds to Eddington luminosity $L_{_{\rm Edd}}=4.3\times 10^{47}$ erg/s. If we follow the mean spectrum of radio-loud quasars (Elvis et al. |
1991). we ect the bolometric Iuniuositv Lj,%οςLOM ere/s based ou the coutimmun (Siebert et al. | 1994), we get the bolometric luminosity $L_{\rm bol}\approx 5.0\times 10^{47}$ erg/s based on the continuum (Siebert et al. |
1996). | 1996). |
Then the accretion rate is roughlya=μμad7A2.010. 2, where Doppler factor D=2.65: here(DIL, we directly used the Doppler factor of the iron [& cinission line as jets. | Then the accretion rate is roughly$ \dot{m} = L_{\rm bol}/(\cd^4L_{_{\rm Edd}}) \approx 2.0\times 10^{-2}$ , where Doppler factor $\cd=2.65$; here we directly used the Doppler factor of the iron K emission line as jet's. |
It sugeests that this object may be powered bv au ADAF. | It suggests that this object may be powered by an ADAF. |
The trausition radius from the standard disk to the ADAF can be obtained by the approximate formula ry©2.6<Late7 for the case that half the released energy is advected [their eq. | The transition radius from the standard disk to the ADAF can be obtained by the approximate formula $r_{\rm tr}\approx 2.6\times 10^3 \alpha^4\dot{m}^{-2}$ for the case that half the released energy is advected [their eq. ( |
£L1) of Narayan Yi 1995]. | 4.1) of Narayan Yi 1995]. |
We get rgzmLOO for a=0.1. | We get $r_{\rm tr}\approx 400$ for $\alpha=0.1$. |
Tf the ejection takes place at LOR, with initial radius Ry= 100. then the deusity is ay=1.95«L0Scun Ὁ LOR,and the temperature is T,=2.3« 10M. Taking the typical values of the parameters. πο=5.0&L0°cm 7 aud T2=5.0& I0"K. for ICAL in the BLR (Netzer 1991). we have the typical expansion timescale ττε2.8 θα, aud the temperature will drop to 10777 K. where Mach uuuber WM?L7«10° from equationCI). | If the ejection takes place at $10R_g$ with initial radius $R_0=10R_g\approx 10^{16}$ cm, then the density is $n_1=1.7\times 10^8$ $^{-3}$ and the temperature is $T_1=2.3\times 10^{11}$ K. Taking the typical values of the parameters, $n_2=5.0\times 10^6$ $^{-3}$ and $T_2=5.0\times 10^7$ K, for ICM in the BLR (Netzer 1991), we have the typical expansion timescale $\tau \approx 2.8\times 10^6$ s, and the temperature will drop to $10^{7\sim 8}$ K, where Mach number ${\cal M}^2=4.7\times 10^3$ from equation (4). |
Theblob's distance from the= center is about JerzS&L«10! ome (3zm 1). | The blob's distance from the center is about $\beta c\tau \approx 8.4\times 10^{16}$ $\approx 80R_g$ $\beta\approx 1$ ). |
It is thus expected that some high cnerev SOR,recombination ues will appear in 2.8< δν since the ejection of a blob | It is thus expected that some high energy recombination lines will appear in $2.8\times 10^6$ s since the ejection of a blob. |
There should be two steps to eject a blob. | There should be two steps to eject a blob. |
The first is the blob formation with the timescale of which is approximate to the viscous timescale (timescale to accumulate matter). namely zzmatr. |r.=1/0,(Ryce)?= 10s at r= Μη. | The first is the blob formation with the timescale of $\tau_{\rm f}$, which is approximate to the viscous timescale (timescale to accumulate matter), namely $\tau_{\rm f} \approx \alpha^{-1}\tau_{_{\rm K}}$ $\tau_{_{\rm K}}=1/\ok=(R_g/c)r^{3/2}=10^6$ s at $r=10$ ]. |
Iu the more accurate global solutiou the radial velocity is higher than the above onc. | In the more accurate global solution the radial velocity is higher than the above one. |
The second is the relativistic ejection with timescale 7. | The second is the relativistic ejection with timescale $\tau_{\rm e}$. |
It seclus reasonable to assume that the timescale of ejection is much shorter than the timescale of blob formation. | It seems reasonable to assume that the timescale of ejection is much shorter than the timescale of blob formation. |
The duration for a blob to produce the iron recombination lines is approximately ty=6.6vrfor T,= 1091 aud n,1.0s10m 3. | The duration for a blob to produce the iron recombination lines is approximately $\tau_{\rm ff}=6.6$yrfor $T_e=10^8$ K and $n_e=1.0\times 10^7$ $^{-3}$ . |
Therefore the uuniber of the blobs producing the recombination line of won I-eumission would be Ny,zmrgí(T|T)€ates.c20 if the ejectionnube takes place at LOR,(It shouldbe noted that this is not the total of the ejected blobs). | Therefore the number of the blobs producing the recombination line of iron K-emission would be $N_b\approx \tau_{\rm ff}/(\tau_{\rm e}+\tau_{\rm f})
\approx \alpha \tau_{\rm ff}/\tau_{_{\rm K}} \approx 20$ if the ejection takes place at $R_g$ (It should be noted that this number is the total of the ejected blobs). |
We assume the | We assume the |
spatial and velocity resolutions, respectively. | spatial and velocity resolutions, respectively. |
We identified 123 cores and estimated the beam-deconvolved radiusReore, velocity width in FWHM corrected for the spectrometer resolutiondu4,, LTE massMoore, virial massM,;,, and mean density of the cores. | We identified 123 cores and estimated the beam-deconvolved radius, velocity width in FWHM corrected for the spectrometer resolution, LTE mass, virial mass, and mean density of the cores. |
Table 2 shows the physical properties of the cores in S140. | Table \ref{propertyTable} shows the physical properties of the cores in S140. |
The definitions of these parameters are the same as those in (2009).. | The definitions of these parameters are the same as those in \citet{ike09b}. |
Here we briefly summarize the parameters specific to this study. | Here we briefly summarize the parameters specific to this study. |
We adopted=22".0 as described in §2,, the antenna efficiency η of 0.4, and the fractional abundance of C180 relative to H5, Xciso of 1.7x1077 (Frerkingetal.1982). | We adopted$= 22''.0$ as described in \ref{observation}, the antenna efficiency $\eta$ of 0.4, and the fractional abundance of $^{18}$ O relative to $_{2}$, $X_{\rm C^{18}O}$ of $1.7\times10^{-7}$ \citep{fre82}. |
. The optical depth of the line in the $140 region has been estimated to be smaller than 1; derived the upper limit of the optical depth of 0.5, from the intensity ratio of the(J—1-0) to C!"O(J—1-0) lines. | The optical depth of the line in the S140 region has been estimated to be smaller than 1; \citet{hig09} derived the upper limit of the optical depth of 0.5, from the intensity ratio of the to $^{17}$ O lines. |
We assumed that the excitation temperature Tex is uniform over the $140 region and is equal to the rotational temperature of 24 K in the NH3 (1, 1) and (2, 2) observations by Higuchietal.(2009). | We assumed that the excitation temperature $T_{\rm ex}$ is uniform over the S140 region and is equal to the rotational temperature of 24 K in the $_{3}$ (1, 1) and (2, 2) observations by \citet{hig09}. |
. In the head clump, the temperature of > 20 K is reasonable because the clump faces the Sh 2-140 H region and numerous young stellar objects have been found (Megeathetal.2004),, as well as the OMC-1 cloud. | In the head clump, the temperature of $>$ 20 K is reasonable because the clump faces the Sh 2-140 H region and numerous young stellar objects have been found \citep{meg04}, as well as the OMC-1 cloud. |
On the other hand, the other two clumps have not been well studied compared to the head clump. | On the other hand, the other two clumps have not been well studied compared to the head clump. |
In the filamentary clump, two IRAS point sources 221924-6302 and 221964-6302 are detected, but the nature of the sources is unknown. | In the filamentary clump, two IRAS point sources 22192+6302 and 22196+6302 are detected, but the nature of the sources is unknown. |
Toward the tail clump, no signature of star formation has been found. | Toward the tail clump, no signature of star formation has been found. |
Although our assumption of the uniform temperature cannot be validated for the two clumps, we found that a low Τε value of 10 K does not seriously affect our discussion, and therefore we adopted the assumption of the uniform Τος in this study. | Although our assumption of the uniform temperature cannot be validated for the two clumps, we found that a low $T_{\rm ex}$ value of 10 K does not seriously affect our discussion, and therefore we adopted the assumption of the uniform $T_{\rm ex}$ in this study. |
We discuss the physical properties of the cores on the basis of comparison with | We discuss the physical properties of the cores on the basis of comparison with |
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