Connections, the market leader on the digital transformation market in Romania, Bulgaria and Serbia, has conducted an analysis of opportunities which Canada, Australia, New Zealand and South-East Asia have when they externalize their IT operations to Romania.
The reduced costs and cultural similarities (Canada), the opportunity of branching out into new markets and access to international know-how (South-East Asia), enhanced productivity because of the time difference and the English language level of the teams (Australia and New Zealand) represent key advantages to externalize the IT&C services to Romania for these regions.
"Roughly 15 per cent of Connections' clients are from Canada and Asia, as well as a plethora of local Romanian corporations and companies. A significant percentage of requests is for Java software developer and IT Infrastructure Engineer. The projects for which we are needed are diverse, from support to infrastructure", stated Bogdan Florea, Connections founder and CEO.
Outsourcing IT services wholly (managed services) or to complete the internal team (staff augmentation) brings a series of key benefits to the company, such as cost reduction for human resources, logistics and offices and productivity increase by using larger teams with reduced costs.
"For the above-mentioned countries, outsourcing to Romania saves up to 25% from the allotted budget of a local team and, as a personal estimate, attracting more customers on ITO from the 3 areas, may bring tens, even hundreds of millions of euro to the Romanian economy", adds Bogdan Florea.
Equally important benefits are fast access to niche specialists and to a dynamic pool of talents, access to current know-how by exposing the team to complex projects at an industrial and geographical level and doing away with downtime periods because the ITO partner is in a region with another time zone and can work in synch with the internal team.
"If the internal team is based in Montreal and works from 10 AM to 6 PM local time, and the externalised team is in Romania works from 8 AM to 5 PM local time, Romania being 7 hours ahead of Montreal, the combined team will be active daily between 1 AM and 6 PM on the Montreal time zone, which reduces downtime by 50%, from 16 hours to only 7 hours," explains Bogdan Florea.
Depending on the complexity of projects there will be teams of 5 to 10 people who can work on 3 projects at the same time.
Connections is a market leader in digital transformation in Romania, with offices in Bulgaria, Serbia and plans to extend at a global level. The company is specialized in IT Outsourcing, Business Process Outsourcing and Software Development. Connections clients are global companies and Romanian medium companies from industries such as Banking, FMCG, Oil &Gas, Telecom and Retail. Starting with July 2018, Connections signed a partnership with UiPath, the Enterprise Robotic Process Automation (RPA) platform with the fastest purchasing at a world level, together with which it successfully implemented automated robotization in key industries. Connections has 300 employees in Romania and in 2007 had a turnover of 4 million euro.


text:
Mortgage Rates Cut By Builders
Michael Corkery and
Dawn Wotapka
Updated March 31, 2009 12:01 am ET
As mortgage rates fall to near historic lows, some home builders are offering even lower interest rates, in an effort to lure buyers amid the slow spring selling season.
The latest sales promotion: Lennar Corp. is offering a fixed 3.625% rate over the life of a 30-year fixed rate mortgage. The deal is besting average rates that have fallen below 5% nationwide, but it comes as other builders are reporting mixed results from similar incentives.
Hovnanian Enterprises Inc. 's recent offer of a 3.99% rate sparked "underwhelming" interest from home buyers, says Dan Klinger, president of the builder's mortgage operation. "It wasn't like we needed crowd control," says Mr. Klinger.
Earlier this year, luxury builder Toll Brothers Inc. was offering a 3.99% interest rate in many of its developments nationwide, but today that rate is no longer available nationally. Toll executives have said that the promotion boosted traffic to its Web site, but the low rate alone hasn't been enough to break weak consumer confidence that is still weighing on the market.
Bargain mortgage rates are the latest sales strategy from builders struggling to sell homes. Mounting unemployment continues dogging the sector, because people without jobs, or those afraid of losing one, are unlikely to purchase, no matter how low the rate.
Since the downturn began, builders have tried everything from free tropical vacations to subsidized closing costs in order to move inventory. They then cut costs and even offered layaway plans for down payments.
For home buyers, the low mortgage rates from the builders represent significant savings. But be wary of the fine print: Lennar is offering the 30-year rate "on select homes," and the loan amount cannot exceed $417,000. The minimum credit score is 700, which is a relatively high score in the current environment. In addition, it could be hard for buyers to come up with the minimum 10% down payment that Lennar requires to qualify for the 3.625% rate.
The builders' low rates may help first-time home buyers, "but it's not going to goose the trade-up market," says Thomas Lawler, a housing economist. "That's because most trade-up buyers use the equity from their previous home for a down payment, and that equity often doesn't exist any more."
KB Home is one builder that isn't chasing buyers with low mortgage rates, for now. Instead, the Los Angeles builder is focusing on offering smaller houses that are competitively priced with foreclosed houses. The strategy seems to be helping KB, which reported on Friday that its sales improved more than some analysts expected.
While some builders acknowledge that price cuts are the most effective way to move inventory, such cuts could cause buyers who have already bought a house at a higher price to walk away from their deposits.
It can be costly for builders to offer the low rates because the companies typically pay mortgage investors cash upfront in exchange for the low interest-rate loans. Federal regulations limit how much the builders can contribute to buy down mortgage rates. Currently, if a home buyer puts down 5% or less, the builder is limited to incentives worth 3% of the sales price, says Mr. Klinger. For downpayments of 10%, the limit climbs to 6%.
Write to Michael Corkery at michael.corkery@wsj.com and Dawn Wotapka at dawn.wotapka@dowjones.com

redpajama_set_name: RedPajamaCommonCrawl


Create unforgettable Las Vegas honeymoon packages with my tips and easy to follow instructions! When I jotted down my ideas for a romantic couple's getaway in the Sin City, I was thinking - how I would like to spend my honeymoon? I've done extensive research, read what people say about romantic hotels and restaurants in Las Vegas with the best views as well as menus, and other stuff interesting to honeymooning couples.
So here is the result - a complete itinerary for a perfect, romantic vacation in the Sin City, as I would love it for myself! I have been married since 1999, but I am thinking of actually following my own instructions to sort of freshen up our relationship, well, if my hubby behaves himself of course!
Considering Vegas is a prime destination for honeymoons as well as for many other events calling for celebration, there is no lack of romantic hotels here! These hotels offer beautiful romantic suites as well as other perks for honeymooning couples.
These hotels would be my next choice for Las Vegas honeymoon ! All of them have something very sweet about them that can be enjoyed by a couple. Paris Hotel, for example, reminds of the most romantic city in the world. The Mirage and Tropicana have a tropical theme so you and your significant other would feel like you are honeymooning in the Caribbean. Platinum Hotel has no casino, but has an amazing spa. It offers a very quiet retreat from all the madness of The Strip, but close enough to it in case you want to have some fun!
Here are five amazing shows in Las Vegas that I would recommend to any couple in a heartbeat! Le Reve is an incredible show with challenging acrobatic stunts and dreamy romantic imagery. Zumanity, also by Cirque du Soleil, is a "naughty" acrobatic show that will heat up your relationship as a couple even more...for at least the night you see the show! Terry Fator is a very talented ventriloquist, and while his show is not quite "romantic", you will get a kick out of his ability to imitate voices and sing with his lips closed! Absinthe is a completely different story...It's a very challenging circus show with stunning acrobatic tricks, mixed with incredibly naughty, at parts vulgar, but very funny adult humor. So leave your inhibitions behind when adding Absinthe to your Las Vegas honeymoon package!
Add a few great live music concerts to your Las Vegas honeymoon package! While the choice of permanent concerts is not as wide as that of other shows, the challenge was to select only the best concerts that you simply can't go wrong with. Therefore, here I only based my selection on popularity of concerts and reviews of other travelers. Enjoy! If you want to see other concerts by touring rock and pop bands, check out the calendar of Las Vegas concerts.
Las Vegas offers plenty of great sightseeing tours, but I wanted to select the most romantic ones. Romance Package is the most straightforward of all Las Vegas honeymoon packages - it includes a romantic gondola ride at the Venetian hotel, tickets to the Wax museum, and a diner at a romantic restaurant! You might also enjoy Photo Tour where you will take a tour with a professional photographer who will be taking memorable pictures of your honeymoon in Las Vegas. Night Lights tour would be perfect for a romantic evening - you will visit top Vegas attractions, lit by neon lights. But perhaps you might more enjoy your Las Vegas honeymoon packages with a Balloon or a Helicopter Ride high above the Strip!
If you want to explore the area a little further - why not to take a day trip? Luckily, there are plenty of possibilities! Here are some excellent destinations located close enough from the city for a quick day trip. Perfect for a Las Vegas honeymoon or a romantic getaway!
If you are a couple who enjoys thrilling, fun or extreme activities - here are some very fun things for you to do in Las Vegas!Las Vegas honeymoon These are the 5 things that I am going to do on my romantic trip to Vegas, so I am sure you would enjoy them during your Las Vegas honeymoon!
When selecting romantic hotels to add to your Las Vegas honeymoon package, I had 2 main criteria in mind: they must have delicious food, and have incredible views. Eiffel Tower Restaurant and Prime Steakhouse at Bellagio offer amazing views of the dancing Bellagio Fountains. Top of the World located on top of the Stratosphere Hotel and Alizé located on top of Palms Casino Hotel have unbelievable views of the Strip. The views from these 2 restaurants are so amazing because Palms is located off the Strip, and Stratosphere is located at the very end (or beginning) of it - so you can see the entire Strip from above! Lakeside at Wynn opens to a very unique "free" show (it's free only to visitors of the hotel) called Lake of Dreams that came straight from the imagination of Steve Wynn - the man behind the design of several amazing hotels in Vegas.
There is only one thing better than a relaxing spa experience - enjoying it with your significant other! I suppose you would love to add spa treatments to your romantic package? The thing about spa in Vegas is that most salons have separate rooms for men and women. But I've found a few that offer a co-ed experience, and even special massage suites and treatment rooms for couples. Great way to honeymoon in Las Vegas!


text:
\section{Introduction\label{intro}}

The measurement of the Galactic rotation curve provides a powerful tool for constraining the mass distribution
in the Milky Way and enters various branches of Galactic kinematics as an essential ingredient.

The measurement of the rotation curve inside the solar orbit at $R_0$ can be done without even knowing the distances to the tracers.
Spectroscopic observations of HI regions and molecular clouds emitting in the radio range yield their line-of-sight velocities,
which under the assumption of the circularity of orbits can be converted to the circular velocities purely geometrically.
Though this technique known as the tangent point method (TPM, \mbox{\citealp{binney}}) provides a quite accurate measurement of the inner rotation curve,
it loses its applicability (1) at small Galactocentric distances $R \, < \, 5$ kpc, where the bar starts to dominate
(however, see \mbox{\citealp{wegg15}} for a recent long bar model)
and therefore the orbits can significantly deviate from
circular ones (\citealp{sofue}) and (2) in the outer disc for $R \, > \, R_0$, where the distances to the tracers cannot be derived from a simple geometry.
And even in the 'good' range of Galactocentric distances $5\,\mathrm{kpc}<R<R_0$, the reliability of the TPM may
be questionable as was shown by recent studies, which consider the spiral structure in galactic discs \mbox{\citep{chemin15,chemin16}}.
In order to probe the outer rotation curve one is obligated to determine distances to the tracers. The distance uncertainties together with the decrease of
tracers' density with increase of R explain why the outer rotation curve is known less confidently than its inner part.
However, very long baseline interferometry (VLBI) provides high-accuracy measurements of parallaxes and proper motions of young star-forming regions and
covers a broad range of Galactocentric distances giving a strong constraint on the shape of the rotation curve \citep{reid14}.
Still, due to the variety of techniques, difficulties in obtaining the accurate 6D dynamical information on coordinates and velocities, change in methodology
at $R=R_0$ if one relies on the TPM inside the solar radius, the rotation curves determined by different authors are not in a perfect agreement with each other \citep{bhawthorn}.

\mbox{\citet{sofue}} presented a comprehensive analysis of previous measurements of the outer rotation curve,
including data for HII regions and C stars, as well as points obtained by the HI-disc thickness method and VLBI observations.
The authors claimed a dip in the rotation curve between 7 and 11 kpc from the Galactic centre, which they attribute
to the presence of a ring of stellar overdensity in the Galactic disc influencing the gravitational potential.
The dip is centred at 9 kpc, where the circular velocity drops by \mbox{$\sim$15 km s$^{-1}$}.
\mbox{\citet{huang16}} also found a similar depression in the rotation curve obtained from stars of the Sloan Digital Sky Survey III's
Apache Point Observatory Galactic Evolution Experiment (SDSS/APOGEE, \mbox{\citealp{eisenstein11}}) and the Large Sky Area Multi-Object Fiber Spectroscopic Telescope (LAMOST)
Spectroscopic Survey of the Galactic Anti-centre (LSS-GAC, \mbox{\citealp{liu14}}).
\mbox{\citet{kafle12}} used blue horizontal branch stars to construct a rotation curve, which also has a dip, although at bigger radii, about 11 kpc.
In contrast to these results, \mbox{\citet{lopez14}}, who studied proper motions of disc red clump giants, obtained a flat rotation curve without any dip,
although the errors still remain substantial.
Having analysed a sample of APOGEE stars covering the range of Galactocentric distances 4-14 kpc, \mbox{\citet{bovy12a}}
arrived at the same conclusion - the authors found that the rotation curve is approximately flat.
Another flat rotation curve was obtained by \mbox{\citet{reid14}} by studying high-mass star-forming regions.

These apparently contradictory results show that a more detailed study of the local Galactic rotation curve is strongly warranted. Now, with the abundant data for distances and
velocities of millions of stars from photometric and spectroscopic surveys of the last decade, the situation is more encouraging.
However, as we show in this paper, the solution of this task is not straightforward: while deriving the mean rotation velocity from the kinematic data,
one has carefully account for the asymmetric drift correction, which itself requires some knowledge or plausible assumptions about the Galactic potential.
Because of this inter-dependence between the input and output we have to approach the problem of the rotation curve reconstruction in an iterative and consistent way.

This paper is organized as follows. Section \ref{samples} describes the data samples and the selection criteria. Section \ref{Jeans} contains the basics
of our analytic approach in the most general form. Then we apply it in two consequent steps. First, we investigate the peculiar motion of the Sun
with the local data from the RAdial Velocity Experiment (RAVE, \mbox{\citealp{steinmetz06}}). This analysis is presented in \mbox{Section \ref{RE}}.
In the second step in \mbox{Section \ref{RC}} we construct the rotation curve of the extended solar neighbourhood using the
sample of G-dwarfs from the Sloan Extension for Galactic Understanding and Exploration (SEGUE, \citealp{yanny09}).
In Section \ref{conclusions} we summarize our findings, discuss dependencies on the assumed constants and parameters and conclude.
Our treatment of the tilt term of the velocity ellipsoid is discussed in Appendix \ref{tracer}.

\section{Data samples\label{samples}}

\begin{figure*}
\centerline{\resizebox{\hsize}{!}{\includegraphics{cmds_h.pdf}}}
\caption{The colour-magnitude diagrams of the whole RAVE and SEGUE G-dwarf data
from 2MASS and SDSS photometry, respectively. The applied cuts are shown in black lines.}
\label{cmds}
\end{figure*}

\begin{figure}
\centerline{\resizebox{\hsize}{!}{\includegraphics{Rz_map.pdf}}}
\centerline{\resizebox{\hsize}{!}{\includegraphics{Vphi_rVphi_pm.pdf}}}
\caption{The spatial distribution of the RAVE and SEGUE samples.
The top panel shows Galactic cylindrical coordinates $R$ and $z$ of the final SEGUE (both thin and thick disc stars) and RAVE data samples (only thin disc stars).
The position of the Sun at Galactocentric distance \mbox{$R_0=8$ kpc} and height \mbox{$z=0$ kpc} is marked with a yellow circle.
The bottom panel shows the whole SEGUE sample projected on the Galactic plane. The value of $\phi=0^\circ$ corresponds to the Sun-Galactic centre axis.
}
\label{samples-plot}
\end{figure}

Our analysis is performed in two steps. Firstly, we re-analyse the determination of the peculiar motion of the Sun and the radial scalelengths
of the three thin disc populations in the framework of the approach of \mbox{\citet{golubov13}}, but based on the most recent data release of RAVE
(DR5, \mbox{\citealp{kunder17}}) and a more careful treatment of the asymmetric drift correction (see \mbox{Section \ref{RE}}).
RAVE is a kinematically unbiased spectroscopic survey with medium resolution (R$\sim$7500),
which provides line-of-sight velocities, stellar parameters, and element abundances for more than 520~000 stars.
In RAVE DR5 improved stellar parameters and abundances were published and \mbox{\citet{McMillan17}} derived new distances taking into account
the parallaxes of the Tycho-Gaia Astrometric Solution (TGAS) from the first Gaia data release (Gaia DR1, \mbox{\citealp{gaia16}}).
Together with the proper motions from UCAC5 (The fifth US Naval Observatory CCD Astrograph Catalog, \mbox{\citealp{zacharias17}}) provided for most of the RAVE DR5 stars,
this sample constitutes the basis of the most reliable local kinematic dataset to date.
From this sample we select stars at Galactic latitudes $|b|>20^{\circ}$ (to avoid the necessity to consider extinction),
belonging to the stripe with $0.75<K-4(J-K)<2.75$ on the colour-magnitude diagram (CMD) constructed with 2 Micron All Sky Survey photometry (2MASS, \citealp{skrutskie06})
(to select the main sequence and have a more uniform population of stars; \mbox{Figure \ref{cmds}}, left panel),
with a signal-to-noise ratio S/N$\geq$30, relative distance errors $\delta d/d<0.5$, errors in proper motions $\delta\mu<10$ mas yr$^{-1}$
and line-of-sight velocities $\delta V_{los}<3$ km s$^{-1}$. To select a cleaner thin disc sample we also use RAVE abundances and take only stars with [Mg/Fe]$<$0.2 \mbox{\citep{wojno16}}.
Our final RAVE sample contains 23~478 stars.
Being very local (Figure~\ref{samples-plot}, top panel), RAVE data cannot be directly employed for the reconstruction of the rotation curve,
but rather are used for the purpose of investigating the solar peculiar motion.

In the second step we use a sample of G-dwarfs from SEGUE, a low-resolution (R$\sim$2000) spectroscopic sub-survey of SDSS.
The sample contains 40~496 G-dwarfs with photometric parallaxes measured by \mbox{\citet{lee11}} with a better than 10-\% accuracy for individual stars.
For our analysis we select stars with signal-to-noise ratio S/N$\geq$30 (to ensure good accuracy of the spectroscopic data),
colour index $0.48\leq g-r\leq 0.55$ (to have a more uniform sample; most stars from the initial sample belong to this colour range anyway),
and absolute magnitude $M_g>4.5$\,mag (which when combined with the colour cut, neatly selects the main sequence; Figure \ref{cmds}, right panel).
We separate the sample into the thin disc with [$\alpha$/Fe]$<$0.25, $|z|<1.5$ kpc and the thick disc with [$\alpha$/Fe]$>$0.25, $|z|<2$ kpc and [Fe/H]$>$-1.2
(to decrease contamination by halo stars).
After applying all the selection criteria, 10~700 stars remain in the thin disc, and 7~040 stars in the thick disc samples.
SEGUE data extend over the range of Galactocentric distances of 7-10 kpc (Figure~\ref{samples-plot}), which makes them suitable for
the local rotation curve analysis.

The tangential velocities $\upsilon_{\phi}$ of the SEGUE stars rely on measurements of line-of-sight velocities and proper motions with distances to individual stars.
Radial velocities and proper motions are obtained by different observational techniques, so they have different
accuracy (about 3 km s$^{-1}$ for line-of-sight velocities and 3-4 mas yr$^{-1}$ for proper motions, which at a distance of 2 kpc from the Sun
converts to a $\sim$ \mbox{30-40 km s $^{-1}$} error)
and might have essentially different systematics. The relative contributions of line-of-sight velocity $\upsilon_{\phi,los}$ and proper motion $\upsilon_{\phi,pm}$ terms to
the resulting tangential velocity $\upsilon_{\phi}$ change with Galactocentric longitude,
so it is important to check that our data when binned in Galactocentric distance are not entirely dominated by one of the terms. The bottom panel of Figure \ref{samples-plot}
shows the SEGUE sample (both thin and thick disc stars selected with our criteria) projected on the Galactic plane.
We calculate and compare the contributions $\upsilon_{\phi,los}$ and $\upsilon_{\phi,pm}$ measured relative to the solar Galactocentric velocity $v_\odot$.
The contribution of the $\upsilon_{\phi,los}$ term is negligible on the axis Sun-Galactic centre, and in other regions values of the ratio reflect an interplay between the direction
and the speed of stellar motions. Importantly, all longitudes are represented in our sample equally well, so in the useful range of Galactocentric distances of 7-10 kpc we expect no bias in $\upsilon_{\phi}$
with respect to the observational techniques.

It's also important to note here that the RAVE data are expected to be kinematically unbiased by construction (see \mbox{\citealp{wojno17}}),
so we do not need to worry about selection effects while working with them. As to the SEGUE \mbox{G-dwarfs}, simple selection criteria were used
to construct this survey \mbox{\citep{yanny09}}, so we expect these data to be relatively free of kinematic bias and therefore we do not include a correction for the selection effects for SEGUE as well.
But as a measure of precaution, before using SEGUE data for the rotation curve reconstruction, we check our RAVE and SEGUE samples for consistency in terms of kinematics
in order to justify our approach (see Section \ref{RE}).

\section{Jeans analysis\label{Jeans}}

In this section we discuss the properties of the asymmetric drift, when applied to a large volume in Galactocentric distance $R$ and
height above the Galactic midplane $z$.
The equation that we are going to formulate here is the basis of our work.

The asymmetric drift is defined as the lag in tangential speed of tracer populations with respect to the rotation curve, $V_a = v_c - \overline{v_{\phi}}$.
The exact value of this quantity depends on stellar population properties and varies with the position in the Galaxy. This implies
that in order to convert mean tangential velocities $\overline{v_{\phi}}$ to the rotation curve, we need to correct them for
$V_a$.
To quantify the asymmetric drift we use the same notation as in \mbox{\cite{golubov13}} and start with the radial Jeans equation for a stationary and axisymmetric system
(in cylindrical coordinates and with negligible mean radial and vertical motion):
\begin{eqnarray}
v_c^2 - \overline{v_{\phi}}^2 &=& -R
\left ( \sigma_{R}^2 \frac{\partial \ln(\nu \sigma_R^2)}{\partial R}
+ \frac{\sigma_R^2 -\sigma_{\phi}^2}{R}
\right.\nonumber\\ &&\qquad\left.
+ \sigma_{Rz}^2 \frac{\partial \ln(\nu \sigma_{Rz}^2)}{\partial z} + F(R,z)
\right ).
\label{JE1}
\end{eqnarray}
Here $\nu$ and $\sigma^2_{R,z,\phi,Rz}$ are the tracer density and velocity ellipsoid,
$\overline{v_{\phi}}$ is the mean tangential speed of the population,
$v_c$ is its circular speed defined in the midplane and $F(R,z)$ measures the vertical variation of the radial force, i.e.,
\begin{equation}
F(R,z) \equiv \left.\frac{\partial \Phi}{\partial R} \right|_z - \left.\frac{\partial \Phi}{\partial R} \right|_0
\quad;\quad v_c^2 = R \left.\frac{\partial \Phi}{\partial R} \right|_{0},
\label{ver_def}
\end{equation}
where $\Phi$ is the total gravitational potential. The right-hand side of Eq. \ref{JE1} is a measure of the asymmetric drift we are interested in.
The last term vanishes at $z=0$, but it should not be neglected at $z\neq0$.
Indeed, as with the increase of height above the midplane the radial gradient of the Galactic gravitational potential decreases,
so does the measured tangential speed.
This effect, if not taken into account, can result in two biases.
Firstly, the derived circular velocity could be underestimated by a few kilometres per second,
causing a shift of the rotation curve as a whole. Secondly, the typical distance of stars from the midplane varies
at different Galactocentric radii due to the sample geometry (see SEGUE sample in Figure \ref{samples-plot}).
This can cause a distortion of the rotation curve, which is unacceptable as the robust reconstruction of the local rotation curve's shape is the very aim of this work.
The second last term is the well-known tilt term, which does not vanish in general even in the midplane (see Eq. \ref{tilt-term} below).
Since these vertical correction terms lead to
a systematic variation of the asymmetric drift increasing with $|z|$, we will take them into account everywhere throughout this work,
even for the relatively local RAVE sample with the range of useful distances limited to $\pm$ 0.5 kpc from the Sun (\mbox{Figure \ref{samples-plot}}, top panel).
The details of the derivation and the assumptions made are provided in \mbox{Appendix \ref{tracer}}.
Here we explain only the essential part of our treatment of \mbox{Eq. \ref{JE1}}.

\begin{table}[b]
\centering

\begin{threeparttable}
\caption{The properties of the Galaxy used for calculations.}
\begin{tabular}{l|l|l} \hline
Variable & Value & Source \\ \hline
$\rho_{h\odot}$ ($M_\odot$ pc$^{-3}$) & 0.014 & (1) \\
$a_{h}$ (kpc) & 25 & \ -- \\ \hline
$M_b$ ($M_\odot$) & 1.1 $10^{10}$  & \ -- \\ \hline
$\Sigma_d$ ($M_\odot$ pc$^{-2}$) & 30 & (1) \\
$h_d$ (pc) & 300 & (1) \\
$R_d$ (kpc)& 2.5 & (2) \\ \hline
$\Sigma_t$ ($M_\odot$ pc$^{-2}$) & 6  & (3) \\
$h_t$ (pc) & 800 & (3) \\
$R_t$ (kpc) & 1.8 &  (4) \\ \hline
$\Sigma_g$ ($M_\odot$ pc$^{-2}$) & 10 & (1) \\
$h_g$ (pc) & 100 & (1) \\
$R_g$ (kpc) & 4.5 & (5) \\
$R_{cut,g}$ (kpc) & 4.0 &  \ -- \\
\hline
\end{tabular}

\begin{tablenotes}
 \item References. (1) \citealp{just10}; (2) \citealp{golubov13}; (3) \citealp{just11}; (4) \citealp{cheng12}; (5) \citealp{robin3}.
\end{tablenotes}

\end{threeparttable}
\label{tab-var}
\end{table}

The rotation curve, which we wish to determine, depends on the same Galactic potential. Therefore, we need to check carefully that we are not
biasing the result implicitly by adopting a special model for the potential, entering \mbox{Eq. \ref{JE1}} through the vertical gradients of tracer density and the radial force.
We use a five-component model of the Galaxy with a spherical Navarro-Frenk-White (NFW) Dark Matter (DM) halo \mbox{\citep{nfw}}
with a local density $\rho_{h\odot}$ and power law slope $\gamma_h=-1$,
a bulge component with mass $M_b$ and three exponential discs for the gas, and the thin and thick disc with local surface densities $\Sigma_i$ and
radial and vertical scalelengths $R_i$ and $h_i$. The gaseous disc has an inner hole with the radius of $R_{cut,g}=4$ kpc.
The values of all used parameters are given in \mbox{Table \ref{tab-var}}.
With this Galactic model we calculate the exact value of
the vertical variation of the radial force using the $GalPot$ code\footnote{Developed by P.McMillan and available at \newline \url{https://github.com/PaulMcMillan-Astro/GalPot}}
(a stand-alone version of Walter Dehnen's GalaxyPotential C++ code, \mbox{\citealp{dehnen98a}}).

In the tilt term in Eq. \ref{JE1} we parametrize $\sigma_{Rz}^2$ as

\begin{equation}
\sigma_{Rz}^2 = \eta (\sigma_R^2 - \sigma_z^2) z/R,
\label{sig_rz}
\end{equation}
where the parameter $\eta$ describes the orientation of the velocity ellipsoid relative to the Galactic centre direction.
The logarithmic derivative of $\eta\nu (\sigma_R^2-\sigma_z^2)$ can be further parametrized with some characteristic scaleheight $h_{\nu \sigma}$
(which describes the vertical variation of the tracer density and velocity ellipsoid orientation and is in general a function of $R$ and $z$), leading to
\begin{equation}
\sigma_{Rz}^2 \frac{\partial \ln (\nu \sigma_{Rz}^2)}{\partial z} =
\eta \frac{\sigma_R^2 - \sigma_z^2}{R}\left[ 1 - \frac{z}{h_{\nu \sigma}}\right].
\label{tilt-term}
\end{equation}

The first term in Eq. \ref{JE1} can be characterized by the radial scalelength $R_E$ (which again may depend on $R$ and $z$), so it reads
\begin{equation}
\sigma_R^2 \frac{\partial \ln(\nu \sigma_R^2)}{\partial R} = - \frac{\sigma_R^2}{R_E}.
\label{term5}
\end{equation}
At this point we remark that under the assumption of a constant disc thickness and a constant shape of the velocity ellipsoid
$\sigma_z^2/\sigma_R^2 $, which implies $\nu \propto \sigma_z^2 \propto \sigma_R^2$, we find $R_E$ related to the radial scalelength of the tracer density
$\nu$ through \mbox{$R_\nu = 2\,R_E = const.$} We will use this assumption later in order to convert the measured $R_E$ into the radial scalelengths
of the subpopulations (see Section \ref{RE}).

Finally, we can write the Jeans equation (Eq. \ref{JE1}) as
\begin{eqnarray}
v_c^2 - \overline{v_{\phi}}^2 &=& \sigma_R^2\left( \frac{R}{R_E}-1\right)  +\sigma_{\phi}^2 \nonumber\\
&& -R\, F(R,z) - \eta \left(\sigma_R^2 - \sigma_z^2\right)\left( 1 - \frac{z}{h_{\nu \sigma}}\right).
\label{JE2}
\end{eqnarray}
This equation is still equivalent to Eq. \ref{JE1}. With a specification of the parameters/functions $F(R,z)$,
$\eta$, $h_{\nu \sigma}$, $R_E$ (\mbox{e.g. $R_E$} independent of $R,z$) we lose generality.

\section{Solar motion and radial scalelengths\label{RE}}

Before using the mean measured relative velocities of the tracer stars to find the mean tangential velocities $\overline{v_{\phi}}$ and
correct them for the asymmetric drift,
we need to correct for the peculiar motion of the Sun $(U,V,W)_\odot$, i.e., to convert the velocities to the local standard of rest.
The determination of $U_{\odot}$ and $W_{\odot}$ from the stellar kinematics in the solar neighbourhood is not a matter of difficulty.
For the radial and vertical components of the solar motion we adopt the values from \mbox{\citet{schoenrich10}}
\mbox{$U_\odot=11.1$ km s$^{-1}$}, \mbox{$W_\odot=7.25$ km s$^{-1}$}, which are also consistent with our data sets.
In contrast, the determination of the tangential component $V_{\odot}$ is challenging.
Due to the fact that the observed tangential motion of stellar populations is affected both
by the solar peculiar velocity and the asymmetric drift, the task of disentangling them poses a problem.
The classical value based on \textit{Hipparcos} data is $V_\odot=5.2$ km s$^{-1}$ \mbox{\citep{dehnen98}}. The more recent and widely used ones
lie approximately between 10 and 12 km s$^{-1}$ (e.g., $12.24 \pm 0.47$ km s$^{-1}$ in \mbox{\citealp{schoenrich10}}). However, among recent estimates there are also
values as high as $\sim$24 km s$^{-1}$ \mbox{\citep{bovy12}} indicating that the local stellar motions could be also influenced by non-axisymmetric Galactic features
like spiral arms \citep{siebert12,monari16} and a bar \citep{dehnen00,monari17,perez-villegas17}.
At the lower limit there is $V_{\odot}=3.06 \pm 0.68$ km s$^{-1}$ found by us previously in \mbox{\citet{golubov13}}.
Rather than taking an old value of $V_{\odot}$ together with the radial scalelengths for three metallicity populations,
we re-determine them here
in order to quantify the impact of our improved analysis in combination with the new distances and improved proper motions.
To find the tangential component $V_{\odot}$ we apply to the local RAVE data the new Str\"omberg relation as in \mbox{\citet{golubov13}}, but now
including the vertical correction terms discussed in the previous section.
We assume a Galactocentric distance of the Sun of \mbox{$R_0=8$ kpc}, which is consistent with \mbox{\citet{reid93}}
as well as with a more recent study by \mbox{\citet{gillessen09}}.
Then adopting the proper motion of Sgr A* from \mbox{\citet{reid05}} we get the solar Galactocentric velocity \mbox{$v_\odot=241.6 \, \pm 15$ km s$^{-1}$}.

Applying  Eq. \ref{JE2} at $R=R_0$ and using \mbox{$v_0 := v_c(R_0)  = v_{\odot} - V_{\odot} $} and \mbox{$\Delta V = v_\odot - \overline{v_{\phi}}$},
we write for the left-hand side:
\begin{eqnarray}
v_0^2 - \overline{v_{\phi}}^2 = (v_{\odot} - V_{\odot})^2 - (v_{\odot}- \Delta V)^2 \nonumber \\
= - \Delta V^2 + 2 v_{\odot}\Delta V - 2 v_{\odot}V_{\odot} + V_{\odot}^2.
\label{lhs2}
\end{eqnarray}
This leads to the new version of the Str\"{o}mberg relation:
\begin{equation}
V^{\prime} = V_{\odot} - \frac{V_{\odot}^2}{2 v_{\odot}} + \frac{\sigma_R^2}{k^{\prime}}
\quad\mbox{with}\quad k^{\prime} =  \frac{2 R_E}{R_0}v_{\odot}
\label{stromberg}
\end{equation}
and the generalized version of $V^{\prime}$:
\begin{eqnarray}
&& V^{\prime}:=\Delta V + \label{Vprime}\\
&& \frac{\sigma_R^2 -\sigma_{\phi}^2 +R_0 F(R_0,z) + \eta (\sigma_R^2 - \sigma_z^2)\left[ 1 - \frac{z}{h_{\nu\sigma}}\right]  -\Delta V^2}{2 v_{\odot}}.\nonumber
\end{eqnarray}

\begin{figure}
\centerline{\resizebox{1.\hsize}{!}{\includegraphics{vel_J-K.pdf}}}
\centerline{\resizebox{1.\hsize}{!}{\includegraphics{AD.pdf}}}
\caption{The recalculation and consistency check of the asymmetric drift correction for the RAVE and local SEGUE data samples.
The RAVE data are recalculated using the improved distances from \mbox{\citet{McMillan17}} and UCAC5 proper motions.
The top panel shows $\sigma_\mathrm{R}$
and $\Delta V$ as functions of (J-K) 2MASS colour for different metallicity bins (compare to Figure 2 in \mbox{\citealp{golubov13}}).
The bottom panel shows $V'$ as function of $\sigma_\mathrm{R}^2$ in view of the new Str\"omberg relation
(Eqs. \ref{stromberg} and \ref{Vprime}) for each metallicity bin. The data points for the local G-dwarfs of SEGUE are added as full circles.
The metallicity binning for RAVE and SEGUE data is identical and has the same colour coding.
Only stars with $7.5\,\mathrm{kpc}<R<8.5\,\mathrm{kpc}$ and in the case of SEGUE with $|z|<1.5$ kpc are selected for the plot.
Dashed colour-coded lines are the linear least squares fit to the RAVE data. Black solid lines are added to readout the
radial scalelengths corresponding to the positions of the SEGUE points and the value of $V_\odot$ determined from RAVE.
Here and later on the error bars are calculated using the observational errors.
}
\label{stromberg-plot}
\end{figure}

To make practical use of Eqs. \ref{stromberg} and \ref{Vprime}, i.e., to determine values of $V_\odot$ and $R_E$, we need to bin our data sample
into sub-bins with different kinematics. For this purpose we separate the RAVE sample in three subpopulations with different metallicities and then bin each subpopulation in
(J-K) colour. The top panel of Figure \ref{stromberg-plot} shows such a binning of the squared radial velocity dispersion $\sigma_R^2$ and
measured velocity $\Delta V$, which can be calculated straightforwardly, without knowledge of $V_\odot$.
One can clearly see that the kinematic properties change systematically with both metallicity and colour.
Using the same binning we plot $V^{\prime}$ versus $\sigma_R^2$ (Figure \ref{stromberg-plot}, bottom panel).
For simplicity, we assume here that $\eta=const.=0.8$ as derived in \mbox{\citet{binney14}} from the RAVE data.
We also treat $h_{\nu\sigma}$ as independent of colour, though differing with metallicity and
select appropriate values from the disc model of \mbox{\citet{just10}} (see Appendix \ref{tracer}).
The height above the midplane $z$ in Eq. \ref{Vprime} is calculated for each metallicity-colour bin as a mean value of the absolute $z$ for individual stars.

As in \mbox{\citet{golubov13}} we still see the systematic difference of $V'(\sigma_{R}^2)$ between metallicity bins,
but the linear dependences show a larger scatter. The assumption that $R_E$, similar to $h_{\nu\sigma}$, is approximately the same for all colours inside
a given metallicity bin, but differs with metallicity, allows us to derive $R_E$ values for the three metallicity subpopulations as well as $V_{\odot}$.
To do so we perform a simultaneous linear fit of the metallicity-colour sequences (shown with colour-coded dashed lines in Figure \ref{stromberg-plot}, bottom panel).
The inverse slopes of the fitting lines $k^\prime_i$ can be directly converted to $R_{E,i}$, which under the assumption of constancy of the disc thickness and the shape of velocity ellipsoid
(see Section \ref{Jeans}) gives us the radial scalelengths for the selected populations. The solar peculiar motion can be readout from the $V^{\prime}$ extrapolated to zero
radial velocity dispersion:
\begin{eqnarray}
R_{d,i} &=& \frac{R_0 k^\prime_i}{v_{\odot}}\\ \nonumber
V_{\odot} &=&  v_{\odot} - \sqrt{v_{\odot}^2 - 2 v_{\odot} \left. V^{\prime}\right|_{\sigma_R^2=0}} \, .
\end{eqnarray}

The updated value of the tangential component of the solar peculiar motion is found to be $V_\odot=4.47\pm 0.8$ km s$^{-1}$,
which translates to the local circular velocity $v_0 \approx 237 \pm 16$ \mbox{km s$^{-1}$}.
The radial scalelengths for the metallicity bins are
$R_d$(0$<$[Fe/H]$<$0.2$)=2.07\pm0.2$ kpc, $R_d$(-0.2$<$[Fe/H]$<$0$)=2.28\pm0.26$ kpc and $R_d$(-0.5$<$[Fe/H]$<$-0.2$)=3.05\pm0.43$ kpc,
which together with $V_\odot$ is in agreement with our old values from \mbox{\citet{golubov13}}.

\ifx
As an attentive reader may notice, one of the terms in $V'$ depends on the solar peculiar motion itself:
$R_0 F(R_0,z)$ includes $v_0$, which depends on $V_{\odot}$ (consider the special case of Eq. \ref{JE2} for $R=R_0$ and the definition of $v_0$).
However, changing the assumed value of $V_\odot$ by 3-4 km s$^{-1}$ influences the results only in the second
decimal place, so we do not need to approach this in an iterative way. To be consistent with our findings, we use \mbox{$V_\odot=4.45\pm 0.8$ km s$^{-1}$}
also for the vertical correction term.
\fi

Now we must check whether SEGUE stars also follow the same trend.
For this purpose we split the thin disc SEGUE sample into the same metallicity bins and consider only stars with Galactocentric distances $7.5<R<8.5$ kpc.
The subdivision in colours is not possible for this data set because of its narrow colour range.
Another characteristic of this sample is that G-dwarfs are distributed over a significantly larger range of $|z|$ (Figure \ref{samples-plot}, top).
And though we do not reconstruct here the shape and orientation of the velocity ellipsoid as a function of $R$ and $z$,
we may roughly account for the vertical gradients of $\sigma_R^2$ and $\sigma_z^2$.
To do so we apply Eq. \ref{Vprime} for the calculation of $V'$ not to the whole metallicity bin, but separately in vertical sub-bins ($|z|=0 \, ... \, 1.5$ kpc with a step of 0.5 kpc)
and calculate the resulting $V'$ by taking a weighted mean of the values obtained for different $|z|$.

The SEGUE points (filled circles in Figure \ref{stromberg-plot}, bottom panel) demonstrate good consistency with the RAVE data, which means that for
further analysis of SEGUE thin disc sample we can securely use the values of scalelengths derived from RAVE.
This is an important result, accounting for all uncertainties of the metallicity calibration in RAVE and possible velocity biases for SEGUE.
To be even more precise we can inverse the problem and read out scalelengths for individual points adopting the solar peculiar velocity derived with the RAVE data.
The values of $R_d$ calculated for the SEGUE data in such a way (see the three solid black lines in Figure \ref{stromberg-plot}, bottom panel) are:
$R_d$(0$<$[Fe/H]$<$0.2$)=1.91\pm0.23$ kpc, $R_d$(-0.2$<$[Fe/H]$<$0$)=2.51\pm0.25$ kpc and $R_d$(-0.5$<$[Fe/H]$<$-0.2$)=3.55\pm0.42$ kpc.
We use these new values and $V_\odot=4.47\pm 0.8$ km s$^{-1}$ in our further analysis.

The linearity of the asymmetric drift correction, i.e., constancy of $R_d$ versus $\sigma_R^2$ is still under debate.
Nevertheless, even if the asymmetric drift dependence on $\sigma_R^2$ in fact turns out to be nonlinear for small $\sigma_R^2$
(as assumed by \mbox{\citealp{schoenrich10}}),
it will correspond to some shift in the measured circular velocity,
but we do not expect this shift to change drastically at different Galactocentric radii.
To the first approximation this would produce only a parallel displacement of the measured rotation curve.
Being interested in the general shape of the rotation curve, not in the exact value of the rotation velocity,
we apply the solar velocity and the radial scalelengths derived by Eq. \ref{stromberg} at all Galactocentric radii.

\section{Asymmetric drift and rotation curve\label{RC}}

Now, with updated values for the solar peculiar velocity and the radial scalelengths for three populations of the selected metallicities,
we proceed to the determination of the rotation curve in the extended solar neighbourhood.
We go back to the Jeans equation formulated for arbitrary $(R,z)$ (see Eq. \ref{JE2}) and apply it to the thin disc SEGUE stars.
In principle, Eq. \ref{JE2} can be directly used for the determination of the rotation velocity as all terms on the right-hand side
are now known and the mean tangential speed can be expressed as $\overline{v_{\phi}} = v_\odot - \Delta V$,
where $v_\odot$ is the tangential speed of the Sun and $(-\Delta V)$ is the mean observed tangential velocity with respect to the Sun.
However, we would prefer to formulate the expression of the rotation velocity in terms of the asymmetric drift $V_a$,
so we recall its definition:

\begin{equation}
V_a = v_c - \overline{v_{\phi}} = v_c(R) - v_\odot + \Delta V.
\label{AD_def}
\end{equation}

Inserting $\overline{v_{\phi}} = v_c - V_a$ into the left-hand side of Eq. \ref{JE2}, we arrive at the quadratic equation for the asymmetric drift:
\begin{eqnarray}
V_a^2 &-&2 v_c V_a  - R \Bigg( F(R,z) + \Bigg. \label{JE_general}\\
&& \Bigg. \eta \frac{\sigma_R^2 - \sigma_z^2}{R}\left[ 1 - \frac{z}{h_{\nu \sigma}}\right]
- \frac{\sigma_R^2}{R_E}
+ \frac{\sigma_R^2 -\sigma_{\phi}^2}{R}
\Bigg ) = 0. \nonumber
\end{eqnarray}
We solve Eq. \ref{JE_general} with respect to $V_a$ and get:
\begin{eqnarray}
V_a &=& v_c(R) - \Bigg\{ v_c^2(R) + R \bigg( F(R,z) + \phantom{\bigg(} \Bigg.\label{Va_root}\\
\Bigg.  \phantom{\bigg(} && \eta \frac{\sigma_R^2 - \sigma_z^2}{R}\left[ 1 - \frac{z}{h_{\nu \sigma}}\right]
- \frac{\sigma_R^2}{R_E}
+ \frac{\sigma_R^2 -\sigma_{\phi}^2}{R}
 \bigg) \Bigg\}^{1/2} \approx \nonumber
\end{eqnarray}
$$
\frac{-R F(R,z) - \eta (\sigma_R^2 - \sigma_z^2)\left[ 1 - \frac{z}{h_{\nu \sigma}}\right]
+ \sigma_R^2\frac{R}{R_E}
- (\sigma_R^2 -\sigma_{\phi}^2)
}{2v_c(R)},
$$
where the last line corresponds to the linear approximation ignoring the $V_a^2$ term.
The difference of the non-linear and linear values for $V_a$ is of the order of 5\% or 1\,km s$^{-1}$.

The final formula for calculating the rotation velocity at radius R for each bin $(R,z)$ is from Eq. \ref{AD_def}
\begin{equation}
v_c(R) = \overline{v_{\phi}} + V_a = v_\odot - \Delta V + V_a
\label{Vc}
\end{equation}
with the asymmetric drift correction $V_a$ given by Eq. \ref{Va_root}.
As $V_a$ is itself a function of $v_c(R)$, the determination of the
rotation velocity is an iterative procedure, during which we assume $v_c \propto R^{\alpha}$.
We start with some small $\alpha$ as initial value, at each step of the iteration the reconstructed rotation curve is fitted and the new value of $\alpha$
is derived to be plugged back in Eq. \ref{Va_root} via $v_c(R)$. The iteration procedure converges very quickly, after two or three cycles.

\begin{figure}
\centerline{\resizebox{1\hsize}{!}{\includegraphics{RC.pdf}}}
\caption{The rotation curve in the extended solar neighbourhood traced via SEGUE stars.
The thin disc stars are split into the same three metallicity bins as before.
For each distance bin the mean rotation velocity $\overline{v_{\phi}}=v_{\odot}-\Delta V$ is measured (dashed curves,
additional binning in $|z|$ applied in the range of $7\,\mathrm{kpc}<R<9\,\mathrm{kpc}$ is not shown here).
The circular velocity (solid curves) is calculated for the three metallicity bins.
The best power-law fit of the form $v_c=v_0(R/R_0)^{\alpha}$ is shown with a black dashed line.
The areas of the \mbox{1, 2 and 3$\sigma$-deviation}
are shown with increasingly lighter shades of grey.
The solar tangential velocity $v_\odot$ is marked with a yellow circle.}
\label{RC-drift-plot}
\end{figure}

\begin{figure}
\centerline{\resizebox{1\hsize}{!}{\includegraphics{Rd_thick.pdf}}}
\caption{The radial scalelength $R_\mathrm{d}$ of the thick disc versus metallicity.
Considered are SEGUE thick disc stars with $7.5\,\mathrm{kpc}<R<8.5\,\mathrm{kpc}$, 4195 in total.
Red points show the radial scalelengths calculated for each metallicity bin with the 'effective' quantities in Eq. \ref{Vprime}.
The points are fitted with a constant and also with $R_d$ linearly dependent on [Fe/H] (solid and dashed lines).
One-sigma areas are shown in grey. The blue point corresponds to the value of scalelength derived in case of binning the same sample
in 4 $|z|$-bins.
}
\label{Rd-plot}
\end{figure}

We bin thin disc SEGUE stars, again separated in three metallicities as before, in Galactocentric distances with equal step of 0.4 kpc.
The further data analysis is not the same for all distance bins. As we mentioned before,
the SEGUE stars are in general distributed over a large range in $|z|$, so we would like to take into account
the vertical gradients in $\sigma_R^2$ and $\sigma_z^2$ by applying our equations separately at different heights for each distance.
As one can see from the top panel of Figure \mbox{\ref{samples-plot}}, such $|z|$-binning for the thin disc sample is justified only close to $R_0$,
approximately for 7\,kpc $<R<$ 9\,kpc, because at larger
Galactocentric distances the majority of stars is located at approximately the same height, such that low-$|z|$ bins would be essentially empty and suffering
from high Poisson noise.
For this reason we do not bin in $|z|$ outside this distance range. Taking this into account, at $R<7$ kpc and $R>9$ kpc
for each R-bin we find the mean tangential velocity $\overline{v_\phi}$ (dashed colour-coded lines in Figure~\ref{RC-drift-plot}),
as well as three velocity dispersions and mean values of $R$ and $|z|$.
Then we apply the correction for the asymmetric drift from Eq. \ref{Va_root}, which is typically $\sim$20 \mbox{km s$^{-1}$}.
For $7\,\mathrm{kpc}<R<9\,\mathrm{kpc}$ we do the same, but separately for three vertical bins (as before, $|z|=0 \, ... \, 1.5$ kpc with a step of 0.5 kpc),
and then calculate the weighted mean $v_c$ at each R.
The obtained rotation curves representing different metallicity bins are shown as solid lines in Figure~\ref{RC-drift-plot} and are broadly consistent with each other
within the error bars.

Between 8 and 10 kpc the rotation curve is flat to an accuracy of a few kilometres per second,
and definitely does not show the 10\,km s$^{-1}$ dip described by \mbox{\citet{sofue,sofue10}}.
On the other hand, the inner part of our rotation curve demonstrates a metallicity-dependent rise with the amplitude up to \mbox{10 km s$^{-1}$},
similar to the one attested by \mbox{\citet{sofue,sofue10}}.

We perform a power-law fit $V_c\propto R^\alpha$ simultaneously to all three rotation curves and find a small power law index $\alpha=0.033\pm 0.034$
(fit shown in Figure~\ref{RC-drift-plot} with a dashed line).
This transforms into the local slope of the rotation curve $dV_c/dR=0.98\pm 1$ \mbox{km s$^{-1}$ kpc$^{-1}$}.
However, the existing measurements of the Oort constants point at a moderately negative slope:
the classical value from \mbox{\citet{binney}} is $dV_c/dR=-2.4 \pm 1$ \mbox{km s$^{-1}$ kpc$^{-1}$},
while the more recent study by \mbox{\citet{bovy17}} from TGAS data suggests an even steeper slope of $-3.4 \pm 0.6$ \mbox{km s$^{-1}$ kpc$^{-1}$}.
Still, we must keep in mind that the Oort constants measure only a very local slope of the rotation curve, which may be stronger perturbed by the local spiral arm structure
and the bar, while our analysis goes all the way to 1-2 kpc away from the Sun.

The thick disc SEGUE stars are not very instrumental in reconstructing the rotation curve,
as the radial scalelength of the thick disc is poorly constrained.
We can solve the inverse problem: use the data to reconstruct the radial scalelength of the thick disc assuming the rotation curve already known.
We express $R_\mathrm{d}$ from Eq. \ref{stromberg} and calculate it for ten metallicity bins of the thick disc.
For the parameter $h_{\nu\sigma}$ of the thick disc we use a value of 800 pc, similar to its scaleheight \mbox{\citep{just11}}.
Furthermore, we take only the local thick disc sample with $7.5\,\mathrm{kpc}<R<8.5\,\mathrm{kpc}$ in order to
avoid regions, where our results can be biased by the uncertainty in the vertical correction term
(this effect is not so important for the thin disc sample, as its stars are in general located at smaller $|z|$ than those of the thick disc).
The resulting $R_\mathrm{d}$ is shown in Figure~\ref{Rd-plot} with red points.
Though the data points show some small variation of $R_d$ with [Fe/H], the constant value of the scalelength \mbox{$2.1 \pm 0.05$ kpc} is more robust
(see the darker one-sigma area in Figure \ref{Rd-plot}). In other words, the chemically defined thick disc behaves as a single kinematically homogeneous population.
The value of the thick disc scalelength found here is consistent with
simulations by \mbox{\citet{minchev15}} and with the data analysis by \mbox{\citet{bovy12}} and \mbox{\citet{kordopatis17}}.
When binning the local SEGUE thick disc sample in metallicity, we calculate $R_d$ for the 'effective' quantities in the bin: velocity dispersions determined for all stars
and also mean $|z|$ and R. Such 'effective' values are quite representative in case of R and velocity dispersions, because our data are very local in terms of Galactocentric distances
and expected to be kinematically homogeneous, so the velocity dispersions should not have a strong gradient in vertical direction. On the other hand, the mean value
of $|z|$ might be misleading as the vertical distribution of stars is quite inhomogeneous. The vertical correction and the tilt term in $V'$ (Eq. \ref{Vprime})
are quite sensitive to $z$, so to cross-check our results we apply Eq. \ref{stromberg} for 4 $|z|$-bins (0...2 kpc with a 0.5 kpc step) with no binning in metallicity as
the data are not abundant enough to allow a simultaneous separation in both $|z|$ and [Fe/H]. The resulting scalelength, which is calculated again as a weighted mean
of the values found for different $|z|$, deviates only slightly from the value
found at the previous step: \mbox{$R_d = 2.05 \pm 0.22$ kpc}. We overplot it in Figure \ref{Rd-plot} with a blue dot for the mean metallicity of the local thick disc sample.
A good agreement between the values of scalelength calculated via the different binning of our sample in the parameter space ensures us of the robustness of the derived result.

\section{Discussion and conclusions\label{conclusions}}

In this paper we performed the revision and improvement of the methods developed previously in \mbox{\citet{golubov13}}.
Starting from the classical Jeans analysis we arrived at the new Str\"omberg relation for the asymmetric drift
and applied it locally to the most recent RAVE data. This enabled us to update the value of the solar peculiar motion to
$V_\odot=4.47\pm 0.8$ \mbox{km s$^{-1}$}. This is lower than the typical values reported by other authors, which are around 10-12 \mbox{km s$^{-1}$}.
However, in the study of \mbox{\cite{sharma14}} also based on the RAVE data,
though in the framework of a different Galaxy model, the solar peculiar velocity is smaller as well, $V_\odot=7.62^{+0.13}_{-0.16}$ km s$^{-1}$.
We also found radial scalelengths for the three metallicity populations, which are
$R_d$(0$<$[Fe/H]$<$0.2$)=2.07\pm0.2$ kpc, $R_d$(-0.2$<$[Fe/H]$<$0$)=2.28\pm0.26$ kpc and $R_d$(-0.5$<$[Fe/H]$<$-0.2$)=3.05\pm0.43$ kpc.
Our analysis demonstrates good consistency of the SEGUE and the RAVE data in terms of kinematics. With the peculiar velocity of the Sun derived from the RAVE sample,
SEGUE data give similar values for the scalelengths,
$R_d$(0$<$[Fe/H]$<$0.2$)=1.91\pm0.23$ kpc, $R_d$(-0.2$<$[Fe/H]$<$0$)=2.51\pm0.25$ kpc and $R_d$(-0.5$<$[Fe/H]$<$-0.2$)=3.55\pm0.42$ kpc.

Then we used the SEGUE sample of the thin disc G-dwarfs to reconstruct the rotation curve of the Milky Way,
ranging from 7 to 10 kpc in Galactocentric radius.
We took into account the asymmetric drift correction (Eq. \ref{Va_root}) and showed that
the resulting rotation curve is essentially flat (Figure~\ref{RC-drift-plot}).
Thus, the existence of any features in the rotation curve just outside the solar radius is discarded in the framework of our analysis.
The formal power-law fit to the rotation curve implies a positive slope $\alpha=0.033\pm 0.034$ consistent with a flat rotation curve,
although we see that its local value is probably smaller. The corresponding
radial gradient of the circular speed is $dV_c/dR=0.98\pm 1$ \mbox{km s$^{-1}$ kpc$^{-1}$}, which is
in agreement with the findings of \mbox{\cite{sharma14}}, who derived a similar value from the RAVE data:
$dV_c/dR=0.67^{+0.25}_{-0.26}$ \mbox{km s$^{-1}$ kpc$^{-1}$}.

Using SEGUE data and relying on the determined slope of the rotation curve, we also calculated the radial scalelength of the thick disc.
It is $2.05\pm0.22$ kpc, and no strong dependence on metallicity was observed.
Values of the quantities derived in this paper are summarized in Table \ref{tab-rez}.

Finally, we have to discuss the dependence of our results on the assumed constants and parameters.

The pair ($R_0$,$v_\odot$), on the one hand, influences the derived stellar spatial distribution and velocities from the observables.
On the other hand, it enters the equation for the asymmetric drift correction (see Eq. \ref{Va_root}).
For the recommended values from \mbox{\citet{bhawthorn}} ($R_0$,$v_\odot$)$=$\mbox{(8.2 kpc, 248 km s$^{-1}$)}
the change in the re-calculated solar peculiar velocity and scaleheights for the three metallicity bins
lie well within one sigma and the changes in the rotation curve can be mostly described in terms of a
vertical shift to higher velocities and horizontal translation to larger Galactocentric distances. Its slope is in this case
$\alpha=0.024\pm 0.031$, which is again consistent with a flat rotation curve.

\begin{table}
\caption{The summary of the results.}
\begin{tabular}{l|l|l} \hline
Quantity & from RAVE & from SEGUE \\ \hline
$V_\odot$ (km s$^{-1}$) & $4.47\pm 0.8$  &  \\
$R_d^\mathrm{thin}$(0$<$[Fe/H]$<$0.2$)$ (kpc) & $2.07\pm0.2$ & $1.91\pm0.23$ \\
$R_d^\mathrm{thin}$(-0.2$<$[Fe/H]$<$0$)$ (kpc) & $2.28\pm0.26$  & $2.51\pm0.25$ \\
$R_d^\mathrm{thin}$(-0.5$<$[Fe/H]$<$-0.2$)$ (kpc) & $3.05\pm0.43$ & $3.55\pm0.42$ \\
$\alpha$ &  & $0.033\pm 0.034$ \\
$R_d^\mathrm{thick}$ (kpc) &  & 2.05 $\pm$ 0.22\\
\hline
\end{tabular}
\label{tab-rez}
\end{table}

What is the impact of the solar peculiar motion?
Changes of $(dU,dV,dW)_\odot$ add quadratically to the corresponding velocity dispersions.
The vertical velocity has no other impact on the result, but we should check that the vertical component of the mean measured relative velocity
of the stars in the sample is approximately $-W_\odot$, which is indeed the case.
$U_\odot$ enters the velocity transformations to cylindrical coordinates, so every time
we change $V_{\odot}$, $R_0$ or $v_\odot$, we have to adapt it to have
$\overline{v_R} \approx 0$ as we assumed in Section \ref{Jeans}. However, this correction is small and we can neglect it
as it is surely beyond the accuracy we can hope to achieve in the framework of our approach. $V_{\odot}$ has a larger impact on the
results as the asymmetric drift correction depends on it, mainly via $v_c$ and the scalelengths (see Eq. \ref{Va_root}).
We test two values of $V_{\odot}$, $\sim$ 3 km s$^{-1}$ \mbox{\citep{golubov13}}
and $\sim$ 7.6 \mbox{km s$^{-1}$} \mbox{\citep{sharma14}}. The rotation curve slope is then
$\alpha=0.039\pm 0.034$ and $\alpha=0.014\pm 0.028$, respectively. We also test the sensitivity of our results to the vertical
scaleheights $h_{\nu\sigma}$ as they are not tightly constrained. Changing $h_{\nu\sigma}$ by $\pm20$\% leads to the slopes of
$\alpha=0.022\pm 0.03$ and $\alpha=0.049\pm 0.038$, which deviate from our standard value by less than 0.5$\sigma$.

To quantify the vertical gradient of the radial force term we assume a Galaxy model, i.e., use some form of the potential as an input.
However, we believe that the rotation curve obtained in Section \ref{RC} is not strongly predefined by this choice.
The $RF(R,z)$ term is not a dominating one in the asymmetric drift correction, so with respect to the rotation velocity it is a first-order correction.
The modification of the potential will enter $v_c$ as a second-order correction only,
and this already meets the limit of our accuracy.
As we inferred by running the tests with the $GalPot$ code, the main contribution to the vertical correction of the radial force
comes from the thin disc, thus its scalelength and scaleheight are the main sources of uncertainty in this term. Taking a $R_{d}$ value of 2 or 3 kpc
we arrive at a rotation curve, which is correspondingly slightly steeper ($\alpha = 0.041 \pm 0.041$) or flatter ($\alpha = 0.027 \pm 0.029$) than the one
we presented in Figure \ref{RC-drift-plot}. Testing $h_z$ of 200 and 400 pc results in similar changes:
$\alpha = 0.041 \pm 0.036$ and $\alpha = 0.026 \pm 0.03$.
The impact of varying $R_d$ and $h_z$ of the other discs is negligible.

None of these deviations from our main result produce essential changes in the derived rotation curve shape. So we can conclude
that in the framework of the developed analysis our outcome is robust with respect to the small changes of our constants
and the pre-choice of the Galactic potential. Our analysis of the local rotation curve does not support the existence of any special features in its shape
like a significant dip at R = 9 kpc.

\section*{Acknowledgements}

This work was supported by Sonderforschungsbereich SFB 881 'The Milky Way
System' (subprojects A6 and A5) of the German Research Foundation (DFG).

Funding for RAVE has been provided by: the Australian Astronomical Observatory;
the Leibniz-Institut fuer Astrophysik Potsdam (AIP); the Australian National University;
the Australian Research Council; the French National Research Agency;
the German Research Foundation (SPP 1177 and SFB 881); the European Research Council (ERC-StG 240271 Galactica);
the Istituto Nazionale di Astrofisica at Padova; The Johns Hopkins University;
the National Science Foundation of the USA (AST-0908326); the W. M. Keck foundation;
the Macquarie University; the Netherlands Research School for Astronomy;
the Natural Sciences and Engineering Research Council of Canada;
the Slovenian Research Agency (P1-0188); the Swiss National Science Foundation;
the Science \& Technology Facilities Council of the UK; Opticon; Strasbourg Observatory;
and the Universities of Groningen, Heidelberg and Sydney.
The RAVE web site is at \url{https://www.rave-survey.org}.

Funding for SDSS-I and SDSS-II has been provided by the Alfred P. Sloan Foundation, the Participating Institutions,
the National Science Foundation, the U.S. Department of Energy, the National Aeronautics and Space Administration,
the Japanese Monbukagakusho, the Max Planck Society, and the
Higher Education Funding Council for England. The SDSS Web Site is \url{http://www.sdss.org}.

UCAC5 proper motions and the distances from \mbox{\cite{McMillan17}} were obtained with the use of
the European Space Agency (ESA) mission Gaia (\url{https://www.cosmos.esa.int/gaia}),
processed by the Gaia Data Processing and Analysis Consortium (DPAC, \url{https://www.cosmos.esa.int/web/gaia/dpac/consortium}).
Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement.

The authors are very grateful to Young-Sun Lee and Timothy C. Beers for providing their SEGUE data sample for our analysis and for fruitful discussions.

We also thank the anonymous referee for the detailed suggestions, which improved the paper significantly.

\bibliographystyle{aa}

redpajama_set_name: RedPajamaArXiv


Freddie Mac said in a press release that their Primary Mortgage Market Survey show mortgage rates have decreased for the third straight week due to disappointing manufacturing data.
Mortgage applications have also decreased slightly from one week earlier data shows.
The 30-year fixed-rate mortgage (FRM) averaged 3.93 percent on the week that ended on Dec. 3, 2015, down from the previous week's 3.95 percent average, according to the press release.
The 15-year FRM averaged 3.16 percent, down from the previous week's 3.18 percent average.
Freddie Mac adds in the press release that the 5-year Treasury-indexed hybrid adjustable-rate mortgage (ARM) averaged 2.99 percent this week, down from the previous week's average of 3.01 percent.
The 1-year Treasury-indexed ARM averaged 2.61 percent this week, up from the previous week's average of 2.59 percent.
Sean Becketti, the chief economist at Freddie Mac, said in the press release that the Treasury yields have decreased by three basis points following weak manufacturing data.
"In response, the 30-year mortgage rate dropped 2 basis points to 3.93 percent," he said. "After the survey closed, Yellen implied that the economy is ready for a rate hike in December."
He adds in the press release, though, that all eyes will be focused on Friday's jobs report, as this will be "the last significant release prior to the FOMC's meeting."
Data from the Mortgage Bankers Association (MBA) show that mortgage applications have slightly decreased.
The market composite index, a measure that shows the total loan application volume, has slipped 0.2 percent, compared to the previous week's data.
The MBA adds that the refinance index also dropped by six percent, compared to the previous week's data while the seasonally adjusted purchase index has risen by eight percent from one week earlier.
The MBA adds, though, that unadjusted purchase index has decreased 28 percent, compared with the previous week.
It was also 30 percent higher than the same week a year ago.


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We're excited to attend the 2019 National Head Start Conference in San Antonio and hope you'll join us. While you're there, visit us at Booth #522 to learn the latest in Conscious Discipline products, events and offerings. Plus, enjoy presentations from Conscious Discipline Instructors on creating the School Family, connecting with relationship-resistant children, communicating with co-workers and more.
The 2019 National Head Start Conference is the largest national event dedicated to all things Head Start. Spend the week exchanging knowledge, sharing achievements, and discussing the latest innovations, developments and obstacles in early childhood. Renew your commitment to providing our nation's most vulnerable children and families with opportunities for success. At the conference, you'll choose from more than 150 sessions and panels, in addition to attending fun events and visiting the nation's largest exhibit hall devoted to Head Start.


text:
the land before time 106
Swarming Leaf Gobblers (The Mysterious Island) appear and eat all of the green food in the Great Valley, forcing the herds to leave. Grandpa Longneck then becomes mortally ill and Littlefoot, along with a young longneck from the herd named Ali, sets out to find the cure: the Night Flower, which grows in The Land of Mists. Narrator: Once upon this same earth, beneath this same sun, long before you... before the ape and the elephant as well... before the wolf, the bison, the whale... before the mammoth and the mastodon... in the time of the dinosaurs. The Land Before Time → The Land Before Time (film) – The franchise has 15+ media topics with more than 10+ films. Showing all 5 items Jump to: Summaries (4) Synopsis (1) Summaries. Even in those circumstances, the non-compliant obligation can attract threats of judicial review. Soon, word gets out that he is trapped in the Mysterious Beyond, urging the gang to set out on a quest to save him. Land Before Time Wiki is a FANDOM Movies Community. Much of the "boilerplate" in section 106 agreements arises from the section itself, as discussed below. George Ball as Daddy Topps 9. He finds out his grandparents have also and it means they must set out and travel to a destination they have not seen. Issac Brown as Chomper 10. We won't set optional cookies unless you agree and enable them. They face dangers such as starvation, Sharptooth, and splitting up. Spoilers. Add an item . Cam Clarke and Elizabeth Daily voice the characters in the TV series, while Scott … Starring: Scott McAfee , Candace Hutson , Heather Hogan , et al. Also Cera learns some news concerning her family: Tria gives birth to a baby named Tricia. Meanwhile, Mr. Thicknose seeks trouble upon Littlefoot, and spills a deep secret, all while a sharptooth follows them. Regulation 122 provides that an obligation may only be taken into account as a reason for granting planning permission where it is: This is now commonly reflected in the wording of the relevant committee report to members, in which the planning officer both confirms that these tests have been considered and sets out the justification for the obligations. The Land Before Time (Davidchannel's Version) The Land Before Time (JamesimusPrime2798) The Land Before Time (CyberChaseZoneFilms2010 Style) Series; Difficulty: Average. 10 questions, rated Average. For more information about these cookies and how they work, please see our Cookies page. Generally speaking, infrastructure to be funded by CIL should not also be secured through section 106 obligations. Unfortunately, the adults blame Doc. Aria Noelle Curzon was born on December 8, 1987 in Hollywood, California, USA. Necessary cookies enable core functionality such as security, network management, and accessibility. Felix Avitia as Littlefoot 2. He must make a difficult decision. This is the only film in the series in which Alec Medlock provides Littlefoot's voice. Ducky is taken captive by Pterano and his henchmen and the gang set out to save her from her captors who have set out to capture the stone of cold fire for themselves. Edit . Healthcare, Digital Health and Life Sciences. Interpretation of Planning Conditions – The Implications. Top tier rankings in this year's legal 500 for national law firm Ashfords. Sections 106(3), (4) and (9) often lead to "boilerplate" clauses in agreements, setting out enforcement provisions, how persons may be released from liability once parting with their interest, and also in the case of s106(9) the formalities required in such instruments. Jeff Bennett as Petrie and Diggers 5. By zebra101. In every film from this one onward, the character has been voiced by a different actor (although Cody Arens voiced the character in every episode of The Land Before Time TV series). They are also attacked by the sharptooth again, and it seemingly dies trying to eat them. The section does not require that all persons interested in the land are required to enter into the obligation. While doing so, they wind up on an island and meet Chomper, a friend they have not seen in a while. 1. Category page. The series began in 1988 with The Land Before Time , directed by Don Bluth and produced by George Lucas and Steven Spielberg . Prime Video From $3.99 $ 3. Further limitations on what may be secured by section 106 obligations arrived in 2010 in the form of the Community Infrastructure Levy Regulations 2010 ("the CIL Regs"). Spike, who has befriended, Tippy, goes with the Spiketails. And when he goes sleep walking one night, the gang has to protect him, but when they lose sight of him, Guido wakes up on top of a sharptooth. History Talk (0) The Cartoon Animated Before Time 14: Journey of the Brave. The Land Before Time (1988) cast and crew credits, including actors, actresses, directors, writers and more. Please note that if you don't then some external applications on our site may not work e.g YouTube video clips. Anndi McAfee as Cera, Petrie's Mother and Diggers 3. The only one you need to be concerned about is the one with the bullies, either II or III of the series. Some Spiketail far walkers visit the Great Valley, and during their visit snow falls upon the Valley. This movie was the last before a break in the then-yearly release schedule of the films, with a two year gap being present between the sixth and seventh films. On what kinds of obligations FANDOM movies Community watching as a kid movies when was. 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text:
Gold Medals: Culinary Olympics Put the Chefs to the Ultimate Test on "Top Chef"
"Welcome back."
No truer words were ever spoken than on this week's episode of Top Chef: Las Vegas ("Culinary Olympics") in which the five remaining chefs faced their toughest challenge--a scaled down mini-version of the famed Bocuse d'Or--before getting cut down to the four chefs who would travel from Las Vegas to Napa for the season finale.
To say that anything was possible is a gross understatement. It literally came down to the wire as the judges decided which of the five was the most relatively weak. To make it this far is no small feat in and of itself, especially given the caliber of chefs this season (overall, anyway) and it was clear that the judges had quite a lot of affection for each of the remaining competitors.
Likewise, this week's installment was also a reminder of just how innately talented each of the remaining chefs is. I can't think of another season where all five remaining chefs were at the same level of skill as they are here. I don't think that the producers would have given them a Bocuse d'Or-like challenge if they didn't think the contestants were up to the challenge.
So how did they perform? Let's discuss.
First, I have to begin by saying how pleased I was that Jennifer got it together this week and was able to put aside her nerves, her exhaustion, or whatever it was that was preventing her over the last few weeks from succeeding in the competition. Her fall from grace was swift but she was able to step it up this week and get back to the Jen we all know and love, delivering confident, thoughtful, and deeply layered (quite literally this week) cuisine.
I'm not quite sure just what went wrong with Jennifer over the course of this competition but it was clear that something was distracting her from focusing on the individual challenges. Whether that was a time issue (she herself indicated last night that she's not quite as swift as the other remaining competitors) or just sheer and utter exhaustion from being put through a physical, mental, and emotional ringer, we'll likely never know.
So when Padma told Jennifer, "welcome back," and did so with a genuine smile, it was a joyful return of the Jennifer Carroll from the early days of the season. I think the taste of Jennifer's seafood ballotine pleasantly surprised Padma in the same way that it did those of us watching at home: it announced that a confident and level-headed Jennifer had returned to Top Chef and that the slips of the past few weeks had been uncharacteristic and wouldn't happen again. In other words: whew.
For their Quickfire Challenge, the chefs were tasked with creating a ballotine, a complicated preparation which essentially means layering a deboned protein inside of protein... inside of protein. (The apex of such a preparation might be the vaunted turducken, in which turkey is stuffed with a duck, which is itself stuffed with a chicken.) But with only ninety minutes, none of these chefs would be insane enough to attempt something as complex as that with the limited time they had.
Here's what they prepared:
Bryan: rack of lamb and Merguez sausage wrapped in caul fat with a medley of purees
Eli: bacon-crusted Scotch egg with a six-minute egg center
Jennifer: calamari steak, scallops, salmon, shiitake, and shiso with rice noodle salad
Kevin: cornmeal-fried fillet of catfish with scallop and shrimp
Michael: "poultry terrine" of chicken with turkey and bacon mousseline
Michael complained that they were never told to actually create a ballotine, but somehow the other four chefs seemed to understand the directions of the Quickfire and delivered dishes that met the brief. Michael did not; his dish was essentially exactly as he described it, a poultry terrine. Which looked beautiful and likely tasted sinfully good but it wasn't what the judges asked for. Bryan's dish looked good but I think he overdid it with the amount of purees on the plate; sometimes less is more and more is just... more.
Eli's Scotch egg looked incredible and he managed to get that six-minute egg just right; he's stuck to his guns this season and produced food that's true to himself and his down-home culinary ethos. I'm glad that he hasn't thrown that out the window to suddenly start cooking in a classical French style or something. The same holds true for Kevin. While his catfish was deemed overcooked, he wasn't defeated or deflated by the criticism and maintained that it was a matter of personal taste.
But it was Jennifer's elegant and refined seafood ballotine that won over the judges, and rightfully so. Due to the use of the calamari, unless it was perfectly cooked, it could have been a rubbery mess of a dish but Jennifer executed it perfectly and walked way with a sizable advantage in the elimination challenge, earning herself an extra half-hour of cooking time.
As for the Elimination challenge itself, I was glad to see that the producers weren't letting the final five contestants rest on their laurels, instead forcing them to compete in a pared-down version of the grueling Bocuse d'Or competition. They'd have to prepare a dish of protein paired with two exceptional accompaniments, all of which would have be served up tableside after being transported to the judges--who included The French Laundry's Thomas Keller, Daniel Boulud, Paul Bocuse, and others--on traditional mirrored platters. And, oh, the winner would get $30,000 and an amazing opportunity, to boot.
I have to say that I was impressed overall with the concept of the dishes overall, even if the execution of the majority of them was found wanting. Granted, this was a difficult challenge of the highest order and there were a lot of moving parts to get under control and the stress of cooking for some extremely respected chefs would have added an additional layer of pressure to the proceedings as well.
So what did the individual chefs offer up? Let's take a look.
Bryan: parsley-crusted lamb loin, lamb shank crepinette with garlic chip, and orzo au gratin with sheep's milk cheese
Eli: sausage-wrapped lamb loin, carrot puree with ras-el-hanout and yogurt foam, and tomato-piquillo canape
Jennifer: unilaterally-cooked salmon and caviar, shrimp flan and black truffles, celery root square and shiitake
Kevin: poached lamb loin, sherry-glazed beet and asparagus in sunchoke cream, red chard
Michael: salmon with cauliflower chickpea tart and zucchini tzatziki
I was a little confused by the judge's reaction to Bryan's dish. At first, they seemed very pleased with the thought and concept behind the dish, even though some of the execution was a little shaky but they seemed to appreciate some of the technical skill he showed with the garnishes (such as that garlic chip). But later at judges' table, they suddenly seemed to be of the mind that the dish wasn't good after all. Huh? What happened in between there? I think he could have gone a little more high-end than the orzo au gratin, which was his play on mac and cheese, but I thought the crepinette looked beautiful and the dish showed cohesion and thought behind it. Bizarre.
Eli's dish, I knew, would land him at the bottom. He did a terrible job of carving that lamb tableside and the fact that he left way too much fat in the loin made it unappetizing and difficult to eat. Which is a shame as his accompaniments looked fantastic. That yogurt cream alone, with the ras-el-hanout-spiced carrot puree was one of the better accompaniments of the night. But I had a feeling that he would be the one to pack his knives and go.
Jennifer, despite having an extra half-hour, still could have done with some more time in this challenge. Her salmon wasn't very evenly portioned, so some pieces ended up being cooked perfectly, while others were overcooked. And her shrimp flan suffered from the same problem: some of the portions were executed perfectly while others weren't, resulting in quality inconsistencies from judge to judge. I do think that her platter was the best looking of the evening and she turned out a gorgeous looking plate. It was just the details that she needed to pay a little more attention to.
Kevin's dish was simple but that was the point: he let the flavors and the quality of the ingredients speak for themselves. I don't think he played it safe at all, as Gail suggested. He decided to sous-vide the lamb loins, which was something he had never done before and he managed to coax a hell of a lot of flavor out of that red chard. Kevin's always been about the ingredients and a rustic simplicity but that's hard to pull off, much less under intense pressure.
As for Michael, I'm not sure what went wrong here. Perhaps it was arrogance or overconfidence. But he delivered one of the most underwhelming dishes of the evening. Sure, it was executed well overall but that cucumber and tzatziki accompaniment was an underseasoned mess and the entire dish lacked any cohesion, despite his efforts to somehow link them with a Mediterranean theme, which sort of fell apart once you looked at the individual elements on the plate. An odd performance, to say the least, as this was really his challenge to lose, given his style of cooking and his technical abilities.
But ultimately, it was Kevin who was crowned the winner of this challenge and earned himself $30,000 along with the chance to compete with the US Bocuse d'Or team, which is a rare honor in itself. And I wasn't surprised when the judges opted to send Eli home. I will admit, however, that I got a little teary-eyed watching Eli cry and say goodbye to his fellow competitors.
Only four chefs remain going into the first part of the season finale. Happy with the Final Four we long ago predicted would ascend to the final rounds? Which chef will emerge victorious? Who will be the next fall before the last challenge? Discuss.
In two weeks on Top Chef: Las Vegas ("Season Finale, Part One"), the contestants leave Las Vegas behind to travel to Napa, where they will complete in challenges (including one aboard the Napa Wine Train) that will winnow them down from four to three before the final competition.
Bravo Top Chef
Labels: Bravo Top Chef
Gotta wonder if Robin somehow had squeaked into the final five, if they still would have had the Elimination Challenge here, since she would have been an embarrassing mess... But also gotta wonder if thats why she was sent home last week, despite Eli's dish last week being horrendous, because at least Eli wouldn't embarrass the show.
Finally the competition heats up with the four best chefs facing off for a spot in the final round. This one should be dramatic... And love all their new haircuts.
Wanted to draw attention to something... Do any od you out there ever get grossed out when Tom shakes the cheftestants hands during prep? I always think - I hope he washes his hands... and it never fails to gross me out.
In fact, in last night's episode, he even wiped his nose when he was talking to one of the brothers, before he went ahead to shake Jen's hand.
Let's hope the editors cut out him washing his hands again. Here's the photographic proof:
http://s74.photobucket.com/albums/i277/rockauteur/?action=view&current=photo-2.jpg
Cassie said…
Ha! That is hysterical (and gross). I love Tom but maybe he should refrain from shaking the contestants' hands from now on...
When Padma told Jen "welcome back" during the quickfire challenge my heart leapt. I've been cheering for Jen since the first episode and it's been awful watching her come so close to elimination these past couple of episode. I hope that after a little rest she will kick some ass in the finale!
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