Datasets:

ReadingTimeMachine
/

rtm-sgt-ocr-v1

Dataset card Data Studio Files Files and versions Community

Split (1)

train · 1.53M rows

Subsets and Splits

No community queries yet

The top public SQL queries from the community will appear here once available.

source stringlengths 1 2.05k ⌀	target stringlengths 1 11.7k
The novelty of this work consists in studying both the CC SN rate and SFR in the same well defined galaxy sample.	The novelty of this work consists in studying both the CC SN rate and SFR in the same well defined galaxy sample.
Thorough the paper we adopt a Hubble constant (Ho) of 75 kkm s! Mpe7! and the Vega System for the magnitudes.	Thorough the paper we adopt a Hubble constant $\rm{H}_{0}$ ) of 75 km $^{-1}$ $^{-1} $ and the Vega System for the magnitudes.
The instantaneous SFR in a galaxy ts directly traced by the number of currently existing massive stars since these stars have short life times.	The instantaneous SFR in a galaxy is directly traced by the number of currently existing massive stars since these stars have short life times.
Usually the total SER in a galaxy is obtained by extrapolating the massive star SFR to lower stellar masses given an initial mass function (IMF) describing the relative probability of stars of different masses forming.	Usually the total SFR in a galaxy is obtained by extrapolating the massive star SFR to lower stellar masses given an initial mass function (IMF) describing the relative probability of stars of different masses forming.
larger evacuated space than model L does (upper left panel), the volumes of space in the very overdense regions 1) are less different between the N and L models, which is because as more and more matter is transferred to the high density regions, there is less and less remaining in the empty regions to be pumped: even though the aggregation of matter into high density regions starts earlier in the N models, it slows down eventually as matter in the low density regions is used up, and there turns out to be time for the L model to catch up somehow.	larger evacuated space than model L does (upper left panel), the volumes of space in the very overdense regions$\delta\gg1$ ) are less different between the N and L models, which is because as more and more matter is transferred to the high density regions, there is less and less remaining in the empty regions to be pumped: even though the aggregation of matter into high density regions starts earlier in the N models, it slows down eventually as matter in the low density regions is used up, and there turns out to be time for the L model to catch up somehow.
These results for our coupled scalar field models (mainly the N models) is similar to that of the ReBEL model (Nusser,Gubser&Peebles2005) as investigated by Keselman,Nusser&Peebles(2010) and Hellwing&Juszkiewicz(2009).	These results for our coupled scalar field models (mainly the N models) is similar to that of the ReBEL model \citep{ngp2005} as investigated by \citet{knp2010} and \citet{hj2009}.
. Having seen above that the fifth force in both the N and C models helps evacuate the low density regions, we now have a look at how the void properties are affected.	Having seen above that the fifth force in both the N and C models helps evacuate the low density regions, we now have a look at how the void properties are affected.
The first interesting quantity is the void volume function (similar to the halo mass function in the studies of the statistical properties of dark matter halos), which shows the number density of voids larger than a given volume V.	The first interesting quantity is the void volume function (similar to the halo mass function in the studies of the statistical properties of dark matter halos), which shows the number density of voids larger than a given volume $V$.
Fig.	Fig.
2 displays our results for the N, C and L models.	\ref{vvf} displays our results for the N, C and L models.
Understandably, the more strongly the matter particles cluster, the more effectively the low density regions are evacuated and therefore the bigger the sizes of the voids tend to be.	Understandably, the more strongly the matter particles cluster, the more effectively the low density regions are evacuated and therefore the bigger the sizes of the voids tend to be.
In the N models, not only does the fifth force, which is unsuppressed, start to take effect earlier, but also the universe expands more slowly, leaving more time for particles to clump (Li&Barrow2010a,b)..	In the N models, not only does the fifth force, which is unsuppressed, start to take effect earlier, but also the universe expands more slowly, leaving more time for particles to clump \citep{lb2010a, lb2010b}.
Consequently, by a=0.5 (Fig. 2,,	Consequently, by $a=0.5$ (Fig. \ref{vvf},
lower left panel), we see large increases in both the void number density and void size in the N models as compared to the L model (for example, the number density could be twice as high).	lower left panel), we see large increases in both the void number density and void size in the N models as compared to the L model (for example, the number density could be twice as high).
Again, as time goes on, low density regions are largely emptied and few particles remain there, then the growth of the voids will slow down.	Again, as time goes on, low density regions are largely emptied and few particles remain there, then the growth of the voids will slow down.
The earlier the evacuation starts, the earlier it will be completed and the growth of voids stops.	The earlier the evacuation starts, the earlier it will be completed and the growth of voids stops.
As a result, when voids in the N models stop growing, those in the L model are still in the process.	As a result, when voids in the N models stop growing, those in the L model are still in the process.
Finally, at a= 1.0, the	Finally, at $a=1.0$ , the
companion.	companion.
We note that the rest of the follow-up elfort reported by Légeretal.(2009). excluded most. but not all. ended. eclipsing binary scenarios.	We note that the rest of the follow-up effort reported by \citet{Leg09} excluded most, but not all, blended eclipsing binary scenarios.
A blend would also give rise to sinusoidal variations at the period ancl phase of the transits Clorresοἱal.2004).	A blend would also give rise to sinusoidal variations at the period and phase of the transits \citep{Kon04}.
. Phere are several cases in the iterature where RV confirmation of transiting planets has oroved (ricky and announcements were made on the basis of marginal RY detections.	There are several cases in the literature where RV confirmation of transiting planets has proved tricky and announcements were made on the basis of marginal RV detections.
Some of these were later shown to »e spurious (Dreizleretal.2003:Ixonacki2003).. while some are widely. considered to remain unsolved (S\WELPS-1 and 11. Sahuetal. 2006)).	Some of these were later shown to be spurious \citep{Drei03,Kon03}, while some are widely considered to remain unsolved (SWEEPS-4 and 11, \citealt{Sah06}) ).
In this context. it is cüllicult o be confident that ColtoT-Tb meets the requirements for planetary confirmation.	In this context, it is difficult to be confident that CoRoT-7b meets the requirements for planetary confirmation.
Let us for now take the measurement of the RV. semi-amplitude of ColtoT-7b at face value. and. estimate. the resulting constraints on its mass. nm.	Let us for now take the measurement of the RV semi-amplitude of CoRoT-7b at face value, and estimate the resulting constraints on its mass, $m_b$.
Figure 7. shows the position of the equiprobability contours in the mass-radius diagram corresponding to our results.	Figure \ref{fig7} shows the position of the equiprobability contours in the mass-radius diagram corresponding to our results.
The most likely value for the density of the planet corresponds to a water/ice composition (orarockycoreandoutbve.g.Rogers&Seager 2010)...	The most likely value for the density of the planet corresponds to a water/ice composition \citep[or a rocky core and a large H/He envelope, as the two are degenerate, as pointed out by e.g.][]{Rog10}.
This composition is marginally favoured (at the ~Le level) over a rocky planet. or a much lighter H2O or Lvclrogen-rich planet.	This composition is marginally favoured (at the $\sim 1\,\sigma$ level) over a rocky planet, or a much lighter $_2$ O or Hydrogen-rich planet.
As the RV detection is marginal. negligible masses (undetectable with the present data) cannot be firmly excluded.	As the RV detection is marginal, negligible masses (undetectable with the present data) cannot be firmly excluded.
Compared το other extra-solar planets. in the 20Mp, range. the updated: position of οτο raises an interesting possibilitv. which was seemingly exeluded by the QUO. value.	Compared to other extra-solar planets in the $20\,M_{\rm Earth}$ range, the updated position of CoRoT-7b raises an interesting possibility, which was seemingly excluded by the Q09 value.
ALL the extra-solar planets in this mass range. including ColtoT-7b. seem most consistent with a composition dominated by water ice. similar to Neptune and Uranus.	All the extra-solar planets in this mass range, including CoRoT-7b, seem most consistent with a composition dominated by water ice, similar to Neptune and Uranus.
The same positions are consistent with a primarily rocky composition with a large gas envelope. but fine-tuning would. be requirecl for such planets to have mean densities identical to those expected. from a Uranus/Neptune-like composition.	The same positions are consistent with a primarily rocky composition with a large gas envelope, but fine-tuning would be required for such planets to have mean densities identical to those expected from a Uranus/Neptune-like composition.
This suggests that those transiting planets. now on very close-in orbits. may all have been formed bevond the snow line.	This suggests that those transiting planets, now on very close-in orbits, may all have been formed beyond the snow line.
ColtoT-Tb could be a mini-Neptune rather than a Super-Earth'.. although such speculation remains subject to the proviso that the confirmation of its planetary nature is not as firm as that of the other planets in the low-mass transiting sample.	CoRoT-7b could be a 'mini-Neptune' rather than a 'Super-Earth', although such speculation remains subject to the proviso that the confirmation of its planetary nature is not as firm as that of the other planets in the low-mass transiting sample.
We have performed a detailed analysis of the LARS observations of ColtoT-7 published by 0090. constructing a realistic model of the activitv-induced stellar signal. making use of all the available data. ancl exploring the possibility of errors bevond the formal RY uncertainties.	We have performed a detailed analysis of the HARPS observations of CoRoT-7 published by Q09, constructing a realistic model of the activity-induced stellar signal, making use of all the available data, and exploring the possibility of errors beyond the formal RV uncertainties.
We find that the signal from stellar activity during the ΗΛ observations can be robustly modelled by dark spots rotating on the surface of the star. using the CCL width ancl bisector information to constrain the model.	We find that the signal from stellar activity during the HARPS observations can be robustly modelled by dark spots rotating on the surface of the star, using the CCF width and bisector information to constrain the model.
We also find clear evidence of svstematics in the RV data. in the form of large jumps (of order 7) which are significantly [larger than the formal uncertaintiesss. ancl are explained neither by activity nor by the putative planetary signal.	We also find clear evidence of systematics in the RV data, in the form of large jumps (of order $^{-1}$ ) which are significantly larger than the formal uncertainties and are explained neither by activity nor by the putative planetary signal.
As these unaccounted-for effects depend strongly on the SNI of the spectra. we attribute them to instrumental uncertainties operating in the mid-SNIU regime. anc which are also seen in other stars observed at similar SNR with LARPS and other high-precision RY spectrographs.	As these unaccounted-for effects depend strongly on the SNR of the spectra, we attribute them to instrumental uncertainties operating in the mid-SNR regime, and which are also seen in other stars observed at similar SNR with HARPS and other high-precision RV spectrographs.
Allowing for the SNlt-dependent uncertainties. we estimate the semi-amplitude of the signal at the period and phase of ColtoT-Tb to be 16+L3mmss +. a detection at the 1.26 level.	Allowing for the SNR-dependent uncertainties, we estimate the semi-amplitude of the signal at the period and phase of CoRoT-7b to be $1.6\pm1.3$ $^{-1}$, a detection at the $1.2\,\sigma$ level.
This value corresponds to a companion mass of my=23+LSAde. with the confidence interval encompassing the fullO Mp range.	This value corresponds to a companion mass of $m_b=2.3 \pm 1.8\,M_{\rm Earth}$, with the confidence interval encompassing the full $\,M_{\rm Earth}$ range.