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1992). | 1992). |
In Fig. 4.. | In Fig. \ref{fxcor}, |
we show the cross-correlation results from the two objects whose spectra are shown in Fig. 2.. | we show the cross-correlation results from the two objects whose spectra are shown in Fig. \ref{spectra}. |
We performed tests with artificially broadened template spectra and different low frequency Fourier. filter cutoffs to assess the accuracy of the task in measuring cy. | We performed tests with artificially broadened template spectra and different low frequency Fourier filter cutoffs to assess the accuracy of the task in measuring $\sigma_{\rm peak}$. |
We found a slightly non-linear relation between input spectral width and width measured byfxcor. | We found a slightly non-linear relation between input spectral width and width measured by. |
. The best agreement was found for a low-frequency cutoff of k=3 (see Fig. 5)). | The best agreement was found for a low-frequency cutoff of k=3 (see Fig. \ref{dispcor}) ). |
We adopted this cut-off for the Fourier filtering. and applied a residual correction as a linear function ofcr — as indicated in Fig. | We adopted this cut-off for the Fourier filtering, and applied a residual correction as a linear function of $\sigma_{\rm obj}$ — as indicated in Fig. |
5 — to the measured width of the science spectra. | \ref{dispcor}
— to the measured width of the science spectra. |
The residual correction is independent of the S/N in the object spectra. which we tested by artificially degrading the broadened template spectra to a range of S/N values between 5 and 35 per pixel. representative for our compact object sample. | The residual correction is independent of the S/N in the object spectra, which we tested by artificially degrading the broadened template spectra to a range of S/N values between 5 and 35 per pixel, representative for our compact object sample. |
From the tests with the template spectra we also found that the background value in the cross-correlation peak fit needs to be kept fixed at 0 (see also Fig. 4)). | From the tests with the template spectra we also found that the background value in the cross-correlation peak fit needs to be kept fixed at 0 (see also Fig. \ref{fxcor}) ). |
Allowing the program to fit the background value led to consistently over-estimated widths, | Allowing the program to fit the background value led to consistently over-estimated widths. |
We accepted a reliable measurement of «pj; for a given object 1f two conditions were met: (1) the average confidence level of the cross-correlation peak was R>4: and (2) none of the template cross-correlations yielded an outlier in the template-object relative velocity. | We accepted a reliable measurement of $\sigma_{\rm obj}$ for a given object if two conditions were met: (1) the average confidence level of the cross-correlation peak was $R>4$; and (2) none of the template cross-correlations yielded an outlier in the template-object relative velocity. |
The first condition removed 9 sources from the main sample of 37 objects while the second condition removed five more sources. | The first condition removed 9 sources from the main sample of 37 objects while the second condition removed five more sources. |
Fig. | Fig. |
| shows that the rejected sources are mostly close to the faint magnitude limit of our survey. | \ref{map} shows that the rejected sources are mostly close to the faint magnitude limit of our survey. |
We note that the two brightest sources with unreliable measurements (see also Fig. 1)) | We note that the two brightest sources with unreliable measurements (see also Fig. \ref{map}) ) |
are those that had been selected as UCD candidates based only on morphology from ACS imaging (ACS Fornax cluster survey. see Jordann et al. | are those that had been selected as UCD candidates based only on morphology from ACS imaging (ACS Fornax cluster survey, see Jordánn et al. |
2007). | 2007). |
Both sources are located within 2’ to the center of NGC 1399 and are the only objects in our target sample whose | Both sources are located within $'$ to the center of NGC 1399 and are the only objects in our target sample whose |
ΠΕ ΠΠ we have whenever possible adopted the same assuniptious that are typically D n xevious models iu the literature (iu particular. the disk-locking models). | simplifying assumptions, we have whenever possible adopted the same assumptions that are typically used in previous models in the literature (in particular, the disk-locking models). |
Our approach in Paper I and is been deliberately systematic. so tlat cach itional component or asstniption in the niocl can be erstoot in turn. | Our approach in Paper I and here has been deliberately systematic, so that each additional component or assumption in the model can be understood in turn. |
Iu this wav. our approach best serves to highheht the influence of he opening of the maneetic ποια due to star-disk. differential rotation (Paper I) aud the fluence of iui accetion-powered stelay wind (present paper). to the previous studies that do not mclude these effects. | In this way, our approach best serves to highlight the influence of the opening of the mangetic field due to star-disk differential rotation (Paper I) and the influence of an acctetion-powered stellar wind (present paper), to the previous studies that do not include these effects. |
We have explored a rauge of conditions that are cosistent with observations of TT Tanzi stars. but we have not explored all of parameter space. and there remai1 uncertainties iuheraut to various adopted assunptious and approximations. | We have explored a range of conditions that are consistent with observations of T Tauri stars, but we have not explored all of parameter space, and there remain uncertainties inherant to various adopted assumptions and approximations. |
Thus. while our quautitative restIts should be viewed as approximate. the results relative o other studies{models in the literature are robust. | Thus, while our quantitative results should be viewed as approximate, the results relative to other studies/models in the literature are robust. |
With this in uind. we compared the precicted equilibriuni spin rate of the APSW scenario to the predictions of two types of disk-locking models. the Ghosh Lamb type aud A-wind models 1). | With this in mind, we compared the predicted equilibrium spin rate of the APSW scenario to the predictions of two types of disk-locking models, the Ghosh Lamb type and X-wind models \ref{sec_comparison}) ). |
Overall. this comparison and our results in general demoustrate that APSWs can explain the observed distribution of voung star spius in a simular wav as the classical disk locking picture. while at the same time avoiding the problem of magnetic field line opening (for the GL-tvpo models). as well as the assumption of spin equilibrimmn aud requirement of significant fiux. trappine (for the N-wind moclel). | Overall, this comparison and our results in general demonstrate that APSWs can explain the observed distribution of young star spins in a similar way as the classical disk locking picture, while at the same time avoiding the problem of magnetic field line opening (for the GL-type models), as well as the assumption of spin equilibrium and requirement of significant flux trapping (for the X-wind model). |
The APSW scenario has one additional parzuneter. the mass loss rate in the wiud. | The APSW scenario has one additional parameter, the mass loss rate in the wind. |
For the assumptions adopted here. we found that in order for the APSWs to have a significant infinence. the mass loss rates should be at least of the order 7 a percent of the accretion rate. | For the assumptions adopted here, we found that in order for the APSWs to have a significant influence, the mass loss rates should be at least of the order of a percent of the accretion rate. |
It still remains to be shown whether aud/or how the energv derived from the accretion process may dive a wind thatis magnetically connected to the star. and with sutiicicutly hieh mass outflow rate. | It still remains to be shown whether and/or how the energy derived from the accretion process may drive a wind that is magnetically connected to the star, and with sufficiently high mass outflow rate. |
Such winds would uot likely be driven significantly bv thermal pressure (duetoarapidcoolingtimeMattPuditz2007). nor by magneto-centrifusal effects (from slowlv-rotatiug stars). but Alfvén waves may be important(e.2007.De-canrpli1981:Ihutiuaunetal.1982:Suzuki ).. | Such winds would not likely be driven significantly by thermal pressure \citep[due to a rapid cooling time][]{mattpudritz07iau}, nor by magneto-centrifugal effects (from slowly-rotating stars), but Alfvénn waves may be important \citep[e.g.,][]{Decampli:1981p2972,
Hartmann:1982p2885, suzuki07}. |
Crammer(2008.2009) demoustrated that Alfvónu waves eoncrated by the accretion process in T Tauri stars are capable of driving enhanced stellar winds. | \citet{Cranmer:2008p1657,
Cranmer:2009p1647} demonstrated that Alfvénn waves generated by the accretion process in T Tauri stars are capable of driving enhanced stellar winds. |
The mass loss rates derived by those models were typically 4X 0.01. | The mass loss rates derived by those models were typically $\chi \la 0.01$ . |
There is a hard energetic upper limit of 4X0.6 foy APSWs (Matt&Puditz2008b).. and. values close to this will have observational consequences that may already be ruled out iu some svstenis (Zaunireira 2011). | There is a hard energetic upper limit of $\chi \la 0.6$ for APSWs \citep[][]{mattpudritz08III}, and values close to this will have observational consequences that may already be ruled out in some systems \citep{zanniferreira11}. |
.. Thus. values of y uch greater than seein uulikelv. iu general. | Thus, values of $\chi$ much greater than seem unlikely, in general. |
Clearly. more work is needed to determine what is the mass loss rate along the stellar maeguetic field aud how this should depend upon system parameters. | Clearly, more work is needed to determine what is the mass loss rate along the stellar magnetic field and how this should depend upon system parameters. |
Measurements of the magnetic ficd streugths of voung stars suegeest that the stellar surface is blauketed with conrplex magnetic fields with a streugths of ~2 kG ([email protected]:Bouvieretal.2007:Jolius-I&xullYane&Johus-I&rull 2011). | Measurements of the magnetic field strengths of young stars suggest that the stellar surface is blanketed with complex magnetic fields with a strengths of $\sim 2$ kG \citep[e.g,.][]{safier98,
Bouvier:2007p3031, johnskrull07, yangjohnskrull11}. |
. Towever. even when complex magnetic felds are preseut. it is the large-scale. (dipole) COlMpolnt that is the most mniportaut for the star-disk interaction aix orques on the star (6.8.Gregoryetal.2008). | However, even when complex magnetic fields are present, it is the large-scale (dipole) component that is the most important for the star-disk interaction and torques on the star \citep[e.g.,][]{gregoryea08}. |
. The dipole couiponeuts have been imieastred via spectropolarimery for at least LO accreting T Tai stars to cate (Donatictal.2007.2008:IDussainet2009:Skell.ALetal.2011).. and the equatorial field strenetls of the dipole com»Olleuts range fron ~1001000 Ci. with the top of this raiice determined by© just1000 two of the stars (DzzGOO Ci for DP Tau. iux B1500 C; or AA Tau: Dou:lotal.2008.201à). | The dipole components have been measured via spectropolarimetry for at least 10 accreting T Tauri stars to date \citep{donatiea07v2129oph,
donatiea08bptau, hussainea09, donatiea10aatau, donatiea10v2247oph,
donatiea11twhya, donatiea11v2129oph, donatiea11v4046sgr,
skellyea11mtori}, and the equatorial field strengths of the dipole components range from $\sim 100-1000$ G, with the top of this range determined by just two of the stars $B_*\approx 600$ G for BP Tau, and $B_*\approx 1000-1500$ G for AA Tau; \citealp{donatiea08bptau,
donatiea10aatau}) ). |
The disk-lockiug uodes usually require field strengths of ~1000€; to explain the slowes rotators. ancl fje weakest equatorial Ποιο, strength we have considered iu the preseut work is D=500€. Th APSW scenario can. in principle. nake up for a weaker maguetic field by having a larger Lass outtlow rate. although the largest values of X considered iu the present paper are already: approaching he upper limits (sec.οιος,Matt&ποτ2008:fun&Ferreira2011). | The disk-locking models usually require field strengths of $\sim 1000$ G to explain the slowest rotators, and the weakest equatorial field strength we have considered in the present work is $B_*=500$ G.The APSW scenario can, in principle, make up for a weaker magnetic field by having a larger mass outflow rate, although the largest values of $\chi$ considered in the present paper are already approaching the upper limits \citep[see,
e.g.,][]{mattpudritz08III, zanniferreira11}. |
. To better constrain the models."n will be iuportaut to have maceic field iieasurenmie articularly of the large-scale couponents. for a larecr siuuple of pre-niain-sequeuce stars. | To better constrain the models, it will be important to have magnetic field measurements, particularly of the large-scale components, for a larger sample of pre-main-sequence stars. |
Iu additiou to those discussed :OVE, there remain a nuniber of caveats to the present work. | In addition to those discussed above, there remain a number of caveats to the present work. |
While we jiwe adopted a relaively sophisticated model for the orques on the star. Wwe Use a sluuplificd treatiment for he accretion history. t1¢ evolution of the maguetic field. and the structure ac evolution of the star itself. | While we have adopted a relatively sophisticated model for the torques on the star, we use a simplified treatment for the accretion history, the evolution of the magnetic field, and the structure and evolution of the star itself. |
Iu QICer to be able to mase a lnore nieanineful comparison with observations. alc especially to be able to evolve the svstem to much later times. it will be necessary to nuprove the theoretlca treatment of these components. | In order to be able to make a more meaningful comparison with observations, and especially to be able to evolve the system to much later times, it will be necessary to improve the theoretical treatment of these components. |
For example. the esent treatiuent of the accretion does not allow for a possible state of the system iu which the disk is truwcated outside of the corotatiou radius. the so calle Loxopelle regumue. | For example, the present treatment of the accretion does not allow for a possible state of the system in which the disk is truncated outside of the corotation radius, the so called “propeller” regime. |
Iu this regine. there is generally no accretion outo the star (ο,1977ο,.Ilar-jonov&Suuvaev1075:Shakura D). OF the accretion is iuteriuitteit (0...Romanovaetal.2005:D'Angelo&Spruit 2010). | In this regime, there is generally no accretion onto the star \citep[e.g.,][]{illarionovsunyaev75, Sunyaev:1977p3829}, or the accretion is intermittent \citep[e.g.,][]{romanovaea05,
DAngelo:2010p3127}. |
. Iu the preseut work. we are considering svstenis with srong maguetic coupling (large maeuctic Prandtl nuuber iu the disk) aud relatively slow rotation. | In the present work, we are considering systems with strong magnetic coupling (large magnetic Prandtl number in the disk) and relatively slow rotation. |
Under these conditions. the maeuetic spidown torque ou the starwhich acts to spin up the disk and can potentially truucate the disk outside of Rov, is relatively weak compared to other torques in the system. | Under these conditions, the magnetic spin-down torque on the star—which acts to spin up the disk and can potentially truncate the disk outside of $R_{\rm co}$ —is relatively weak compared to other torques in the system. |
Tls. we dont expect the propeller regime to © muüportant for most of the evolution these svstenis. | Thus, we don't expect the propeller regime to be important for most of the evolution these systems. |
However. there may be times in the history ot such stars (o.g.. toware the eud of the accretion phase) 1i which the xopeller reeiue Is inportaut or the angular 1iomoentuni oss. | However, there may be times in the history of such stars (e.g., toward the end of the accretion phase) in which the propeller regime is important for the angular momentum loss. |
Properv capturing the transition between accreting and propeller sates requires a self-cousisteu treatinent of the evolutioi of the ποσοlon disk (asiue.ThAr-uitaee&€‘larke199€xD’AnecloSpruit 2010 | Properly capturing the transition between accreting and propeller states requires a self-consistent treatment of the evolution of the accretion disk \citep[as in, e.g.,][]{armitageclarke96,
DAngelo:2010p3127}. |
).. the xeseut model. we imposed the accretion rae onto the star. which nuMieitlv assumes that the disk js alwavs able to transport excess angular momentum given to it w the star (sec.eB.the.Matt&Pudritz 2005)). | In the present model, we imposed the accretion rate onto the star, which implicitly assumes that the disk is always able to transport excess angular momentum given to it by the star \citep[see, e.g.,][]{mattpudritz05}. |
. To explore he influence of propeller regime on the long-term spin evolution. future models should include both self disk evolution aud sophisticated treatineut of he torques on he star. | To explore the influence of the propeller regime on the long-term spin evolution, future models should include both self-consistent disk evolution and sophisticated treatment of the torques on the star. |
actually detected at one pass will be ry=piN: since neither quantity on the right is known. we cannot calculate the other. | actually detected at one pass will be $n_1 = p_1N$; since neither quantity on the right is known, we cannot calculate the other. |
On a second pass (or with a different. survey). similulv. na=poN will be detected. allowing for the fact that the probability may. change: and οἱ course (he particular set of objects will diller in general. with an overlap of 23. | On a second pass (or with a different survey), similarly, $n_2 = p_2 N$ will be detected, allowing for the fact that the probability may change; and of course the particular set of objects will differ in general, with an overlap of $n_3$. |
If we assume the first set of detections nq is a random sample of the parent population. the probability of detection by the second survey is just po=na/n4. | If we assume the first set of detections $n_1$ is a random sample of the parent population, the probability of detection by the second survey is just $p_2 = n_3/n_1$. |
Working backwards we can now calculate py and N. | Working backwards we can now calculate $p_1$ and $N$. |
I the two probabilities are sienilicantlv different. we should start. looking Lor svstematic differences between the detected objects. | If the two probabilities are significantly different, we should start looking for systematic differences between the detected objects. |
Looking al the number of candidate objects in this way. things are less encouraging than with the plate grading. | Looking at the number of candidate objects in this way, things are less encouraging than with the plate grading. |
36 were recorded both times: 20 only in 1997; ancl 31 only in 2000. | 36 were recorded both times; 20 only in 1997; and 31 only in 2000. |
Taken al [ace value. il seems (hat an object matching our morphological criteria has slightly over half a chance. certainly not as much as two-thirds. of even being seen. | Taken at face value, it seems that an object matching our morphological criteria has slightly over half a chance, certainly not as much as two-thirds, of even being seen. |
But on a third examination of these fields we found Chat. of the 1997-0nlv objects. 17 were really too bright and small to fit the criteria: and of the 2000-only objects. 26 were actually too much like Galactic nebulositv to be worth recording. | But on a third examination of these fields we found that, of the 1997-only objects, 17 were really too bright and small to fit the criteria; and of the 2000-only objects, 26 were actually too much like Galactic nebulosity to be worth recording. |
What happens is this: in each examination we were anxious not to miss any (rue Local Group clwarls. aud so included many doubtful objects. | What happens is this: in each examination we were anxious not to miss any true Local Group dwarfs, and so included many doubtful objects. |
Between the two examinations there was a shift in whieh doubtful objects we were inclined to include. | Between the two examinations there was a shift in which doubtful objects we were inclined to include. |
A second look at each candidate showed that many were Clearly not of interest. and that we were choosing good candidates much more reliably. | A second look at each candidate showed that many were clearly not of interest, and that we were choosing good candidates much more reliably. |
If we include only good objects we come up with a one-pass reliability approaching90%. | If we include only good objects we come up with a one-pass reliability approaching. |
. This is probably optimistic. however. since it only compares one set of eves with itself. | This is probably optimistic, however, since it only compares one set of eyes with itself. |
To get a better comparison we need another set of eves. | To get a better comparison we need another set of eyes. |
We are aware of only one other survey comparable to ours. (hat is. which examined photographic material over the entire skv (or a large Iraction of it) in seach of Taint objects with the morphology of dwarl galaxies. | We are aware of only one other survey comparable to ours, that is, which examined photographic material over the entire sky (or a large fraction of it) in seach of faint objects with the morphology of dwarf galaxies. |
As reported by Karachentsevοἱal. (2001).. their results along with those of Karachentseva&Ixarachentsev(1998): IXarachentsevοἱal. (1999):: IXaraclientsevοἱal. (2000) ancl Karachentseva&IKarachentsey(2000) covered of the skv looking for dwarl galaxies in the Local Volume (out to a few megaparsecs). using film copies of the ESO/SRC and POSS-L plates. | As reported by \citet{KKH01}, , their results along with those of \citet{KK98}; \citet{KKR99}; \citet{KKS00}; and \citet{KK00} covered of the sky looking for dwarf galaxies in the Local Volume (out to a few megaparsecs), using film copies of the ESO/SRC and POSS-II plates. |
While their criteria were slightly different (for example. they included objects down to half an are minute in size. which of course reasonable if one is interested in (hines farther away than the Local Group) they should have included our criteria as asubset. | While their criteria were slightly different (for example, they included objects down to half an arc minute in size, which of course reasonable if one is interested in things farther away than the Local Group) they should have included our criteria as asubset. |
withh a ring of atomic (HI) gas. | h a ring of atomic (HI) gas. |
number of publications starting in the 1980s has focused on the molecular gas in L1535 and the larec-scale environment (ος.TT). | number of publications starting in the 1980s has focused on the molecular gas in L1535 and the large-scale environment \citep[e.g.][]{1982A&A...111..339U,1984ApJ...283..140G}. |
After the identification of an LRAS source associated with this cloud. (??7).. the object has been analvsed in the infrared domain (e.g.7) and in the submm/mm continuum (e.g.2?7?7).. tracing the dust in the system. | After the identification of an IRAS source associated with this cloud \citep{1988MNRAS.235..139P,1991MNRAS.251...63P}, the object has been analysed in the infrared domain \citep[e.g.][]{1994ApJS...94..615H} and in the submm/mm continuum \citep[e.g.][]{1991ApJ...382..555L,1996ApJ...466..317O,1996A&A...309..827S}, tracing the dust in the system. |
HU0X504325 was found to harbour a protostar with subsolar luminosity and a disk seen at high inclination (??).. embecced in a cloud core with a ciameter of several tens of thousands of AU. | IRAS04325 was found to harbour a protostar with subsolar luminosity and a disk seen at high inclination \citep{1993ApJ...414..676K,1993ApJ...414..773K}, embedded in a cloud core with a diameter of several tens of thousands of AU. |
In addition. large-scale outflow: activity has been identified (e.g.2?7).. | In addition, large-scale outflow activity has been identified \citep[e.g.][]{1987ApJ...321..370H,1992ApJ...400..260M,2001AJ....121.1551W}. |
Phe source is established as a prototypical small-scale site of star formation. | The source is established as a prototypical small-scale site of star formation. |
Until 1999. the structures within the LRAS bean have not been resolved. which results in various problems. | Until 1999, the structures within the IRAS beam have not been resolved, which results in various problems. |
The near-infrarecl images clearly show a bright. nebulosity. indicating that the fluxes from LRAS ancl single-clish observations are contaminated. by extended: emission. | The near-infrared images clearly show a bright nebulosity, indicating that the fluxes from IRAS and single-dish observations are contaminated by extended emission. |
As a result. the properties of the central source ancl its close environment are poorly constrained. | As a result the properties of the central source and its close environment are poorly constrained. |
Confusingly. the direction of one of the large-scale outflows does not. agree with the orientation of the infrared. nebulosity. interpreted as outflow cavity. as pointed out by 2.. | Confusingly, the direction of one of the large-scale outflows does not agree with the orientation of the infrared nebulosity, interpreted as outflow cavity, as pointed out by \citet{1993ApJ...414..676K}. |
2. presented LIST imaging of the object. revealing complex. substructure. | \citet{1999AJ....118.1784H} presented HST imaging of the object, revealing complex substructure. |
In particular. the images show the presence of a second. well-separated point. source (115N804325C. which has à resolved disk seen edge-on. | In particular, the images show the presence of a second well-separated point source (IRAS04325C), which has a resolved disk seen edge-on. |
Ehe main light source LRASOL325AB is speculated to be a binary. | The main light source IRAS04325AB is speculated to be a binary. |
In. addition there are. various scattered light features. | In addition there are various scattered light features. |
Originally Cucled by the suspicion the second: source IRASO4325C might be a proto brown cwarl we have conducted our own observations of the system. | Originally fueled by the suspicion the second source IRAS04325C might be a proto brown dwarf, we have conducted our own observations of the system. |
In our first paper (2).. we detect the second component with mmm. interferometry and show the first infrared spectrum for this object. | In our first paper \citep{2008ApJ...681L..29S}, we detect the second component with mm interferometry and show the first infrared spectrum for this object. |
Llere we present a comprehensive dataset for the full IRASO4325 system. including new near- ancl mid-infrared imaging. near-infrared. spectroscopy for both components. and submillimeter interferometry. | Here we present a comprehensive dataset for the full IRAS04325 system, including new near- and mid-infrared imaging, near-infrared spectroscopy for both components, and submillimeter interferometry. |
We consistently assume a distance of ppc for the Taurus star forming region (?) when converting from apparent to physical separations. | We consistently assume a distance of pc for the Taurus star forming region \citep{2007ApJ...671..546L} when converting from apparent to physical separations. |
A physical distances are given in projection against the plane of the sky and should be seen as lower limits to the actual distances. | All physical distances are given in projection against the plane of the sky and should be seen as lower limits to the actual distances. |
eear-nfrared. images in J-. H-. and Ix-band. were taken on the 23 August 2008 with the NIHRI camera (2). at the Gemini-North. nimtelescope! ALL Gemini observations or HILASO4325. were taken in queue mode in the band-2 »ograni GN-2008B-Q-73. | Near-infrared images in J-, H-, and K'-band were taken on the 23 August 2008 with the NIRI camera \citep{2003PASP..115.1388H} at the Gemini-North m. All Gemini observations for IRAS04325 were taken in queue mode in the band-2 program GN-2008B-Q-73. |
We used the [/6 camera with a scale of 112/pix and 1207« FOV. | We used the f/6 camera with a scale of 12/pix and $120" \times 120"$ FOV. |
X T-step dither xutern was carried out in cach band. with 15 offsets and lÜssec integration time per position. | A 7-step dither pattern was carried out in each band with 15" offsets and sec integration time per position. |
The total on-source ime in each band was ssec. | The total on-source time in each band was sec. |
The seeing measured [rom 1-3 well-detected point sources outside LRASOL325 was 0755. | The seeing measured from 1-3 well-detected point sources outside IRAS04325 was 5. |
The reduction of the NURI J-. H- and Ix-band images ooceeded: as. follows: a sky image for each [filter was created using the dithered science images. | The reduction of the NIRI J-, H- and K'-band images proceeded as follows: a sky image for each filter was created using the dithered science images. |
The sky was then subtracted to cach science. image using the ESO. eclipse xickage (2)... | The sky was then subtracted to each science image using the ESO eclipse package \citep{1997Msngr..87...19D}. |
We carried out a Uatheld correction using domellats. | We carried out a flatfield correction using domeflats. |
Phe alignment and coadedition of the images was done with the programs Scamp (?7) ancl Swarp (2?) to xoduce the final science stacks. | The alignment and coaddition of the images was done with the programs Scamp \citep{2006ASPC..351..112B} and Swarp \citep{2002ASPC..281..228B} to produce the final science stacks. |
In the same Gemini program. we obtained L'- jum) ancl ΝΕΡας (4.7) images with NIRS [25 camera (Q'O02/pix) and a FOV of 22.4.22.47. | In the same Gemini program, we obtained L'- $\,\mu$ m) and M'-band $\,\mu$ m) images with NIRI's f/32 camera 02/pix) and a FOV of $22.4" \times 22.4"$. |
In the E-band a ive step dither pattern. with 3 olfsets was executed. twice with 20 σαο Pssec exposures at each position. which gives a total on-source time of 200ssec. | In the L-band a five step dither pattern with 3" offsets was executed twice with 20 coadded sec exposures at each position, which gives a total on-source time of sec. |
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