text:
Publications of HSE
О динамике институтов гражданского общества в Нижегородской области и Санкт-Петербурге. Гражданское общество и некоммерческие организации
National Research University
HSE Academic Journals
HSE Publishing House
HSE Working Papers
HSE Data Books
business informatics
IT and mathematics
state and public administration
Mechanics and Mechanical Engineering
Chemical Technologies
Materials Technologies
Effective Natural Resource Management
Environmental Biotechnologies
Industrial Biotechnologies
Medicat and Health Sciences
Medical Biotechnologies
Agriculture, Forestry, and Fisheries
Livestock and Dairy Farming
Agricultural Biotechnologies
Economics and Management (including Public Administration)
Sociology (including Demography and Anthropology
Political Science (including International Relations)
Social and Economic Geography (including Urban and Transportation Studies)
History and Archeology
Philology and Linguistics
Philosophy, Ethics, and Religious Studies
State Capacity: How It Is Measured and Compared
'State capacity' refers to a state's ability to make and effectively implement decisions in domestic and foreign policy. In a study, HSE University political scientists evaluated the state capacity of 142 countries. Based on their findings, the researchers created and trialed a state capacity index, identified eight models of state capacity, and compiled a general international ranking.
Introduction to Daurian Gothic: What It Is and How It Has Emerged in Transbaikalia
Medieval horror, vampires, sorcerers, mysterious monks and the rising dead, alongside real historical figures and stories about the Russian Civil War wrapped in the aura of mysticism – this is perhaps the shortest formula for Daurian Gothic. Alexei Mikhalev, Doctor of Political Science, discusses this phenomenon and its evolution.
HSE Scholars Propose New Method for Measuring Individual Well-being
Their initial tests were carried out with football fans, by measuring their emotional state. It turned out that, on average, uncertainty about a match result can increase the probability of unhappiness by 13.6%. The results of this study were published in the Journal of Happiness Studies.
Chapters of books
Report a publication
Research at HSE
С. 241-262.
Сунгуров А. Ю., Распопов Н. П., Погорелова С. А.
The concept of civil society has taken on a new dimension in connection with the development of the sector of non-profit organizations, or "the third sector". Under the non-profit (third) sector is the collection of the (system of) population groups and organizations, do not put before ourselves the purpose of increasing personal income directly through participation in the work of such groups and organizations or through their ownership of (non-profit organisations or NGOs). The main function of such organizations is, to one degree or another, the expansion of the limits of freedom and empowerment of the population of authority, involvement of the public in the process of social change, the development of social protection.
Full text (PDF, 487 Kb)
Keywords: civil societynon-profit organizationsdynamics of NGOs
In book
Регион в период модернизации: стратегии развития: материалы Международной научно-практической конференции, 20 апреля 2012 г.
Edited by: Д. А. Шпилев Н. Новгород: Издательство НИСОЦ, 2012.
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Анализ эффективности некоммерческих ассоциаций методом стохастической границы (на примере товариществ собственников жилья)
Борисова Е. И., Пересецкий А. А., Полищук Л. И. Прикладная эконометрика. 2010. № 4(20). С. 75-101.
The paper demonstrates the potential of the stochastic frontier-based methods of performance assessment of non-profit associations. They are commonly used for productivity analysis and could serve as an adequate tool for such assessment, especially when dealing with numerous non-profits pursuing identical and clearly identified objectives. A case in point are homeowners associations (HOA), which are formed within apartment buildings to manage common property. Data was collected by a survey of 82 HOAs in Russias national capital Moscow and a large industrial city of Perm. Different techniques and robust checks are applied, exogenous parameters that influence HOA efficiency are revealed. Among those, physical conditions of the housing stock and ability of tenants to resolve the collective action problem in operating housing infrastructure were shown to be of primary importance. Overall, HOA, despite of their appeal and successful performance in developed nations, are not necessarily a superior option in countries and societies where civic capacity is in short supply, and housing stock suffers from wear and tear.
Russians' participation in cash donations: factors and level of involvement
Mersiyanova I. V., Ivanova N., Korneeva I. Sociology. SOC. Высшая школа экономики, 2014. No. 53/SOC/2014.
As part of Russia's transformation process of the last decade, the preconditions for the emergence of philanthropic institutions were created. A plethora of evidence illustrates how this process has unfolded. However, there is a limited amount of research devoted to the philanthropic activity of Russians. This deficit stems from a lack of empirical data on the subject. This article seeks to partly rectify this deficit of empirical information on the topic. We examine the level of involvement of Russians in making cash donations and reveal the factors that influence it. Empirical data were collected within the framework of the monitoring of Russia's civil society that has been conducted since 2006.
Коммуникативные и социальные аспекты возрастания роли репутации в современном российском политическом процессе
Коган Е. В. Социум и власть. 2010. № 4. С. 38-42.
The article is devoted to analysis of concepts reputation and reputation management in conditions of modern Russian political reality. The author tries to determine positions of reputation communications in political sphere of Russia, which have a goal of social trust (base of strong civil society) development.
Свобода от эксплуатации - политической, социальной, экономической, трудовой, служебной, корпоративной, контрольной: проблема ее уголовно-правового обеспечения
Панченко П. Н. Аграрное и земельное право. 2011. № 3. С. 81-88.
There are analyzed the encountered in the title kinds of exploitation, uncovered its social danger and given the criminal legal characteristics, pointed out the ways of counteraction in the article. The author substantiates the conclusions concerning the freedom from such kinds of exploitation and the measures of combating encroachments on this freedom. There is shown the significance of the civil society institutions for the relevant areas of penal policy.
Институты взаимодействия государственной власти и гражданского общества в Санкт-Петербурге и Нижнем Новгороде
Сунгуров А. Ю., Распопов Н. П., Захарова О. С. и др. В кн.: Культура конфликта во взаимодействии власти и гражданского общества как фактор модернизации России. М.: ИД "Ключ-С", 2012. С. 175-184.
Общество до общественности: "общество" и "гражданское общество" в культуре российского Просвещения
Каплун В. Л. В кн.: От общественного к публичному: Коллективная монография. СПб.: Европейский университет в Санкт-Петербурге, 2011. С. 395-486.
Концепты третьего сектора и гражданского общества в контексте теорий демократии, управления и экономического развития.
Тарасенко А. В. Центр исследований модернизации. Серия препринтов. Европейский университет в Санкт-Петербурге, 2014
Профессионализация фандрайзинга в современном российском обществе
Сурина М. А. В кн.: Профессии социального государства. М.: ООО «Вариант», ЦСПГИ, 2013. С. 308-325.
Культура конфликта во взаимодействии власти и гражданского общества как фактор модернизации России
Никовская Л. И. М.: ИД "Ключ-С", 2012.
A Critical Appraisal of the Conceptualization of Public Park and Recreation Marketing
Novatorov E. V. SSRN Working Paper Series. Social Science Research Network, 2012. No. 2133237.
The objectives of the study were (a) to identify the reasons and concerns of those public administrators and marketing scholars who do not accept the usefulness of marketing in the public sector; (b) to deconstruct, comprehend, interpret, and critically appraise the current conceptualization of public sector marketing from the viewpoint of negativists identified in step (a); and (c) to reconstruct, redefine, reinterpret, and reoperationalize the current controversial conceptualization of public sector marketing into a new conceptualization in the context of park and recreation services. The critical theory approach to the study primary used non-empirical procedures data collection and analytic procedures which included investigative research, negative case analysis, and theoretical triangulation. These procedures were supplemented with empirical data collected from in-depth interviews with five scholars and with three parks and recreation managers. Results of the non-empirical procedures revealed the biased selective nature of the current conceptualization of public park and recreation marketing and the existence of alternative conceptualizations which have been ignored. The existing and alternative models were discussed with scholars and park and recreation managers. Support was found for the alternative models. From these data an alternative conceptualization of public park and recreation marketing was developed and named the concept of administered marketing. Implications for park and recreation managers are discussed. Directions for future research into the administratively managed park and recreation marketing concept are suggested.
Civil Society Awakens? The Systemic and Non-Systemic Opposition in the Russian Federation: National and Regional Dimensions
L.: Ashgate, 2015.
ISTR Conference Working Papers
Vol. VII. Istanbul: The International Society for Third-Sector Research, 2012.
"Facing Crises: Challenges and Opportunities Confronting the Third Sector and Civil Society" 9th International Conference of the International Society for Third Sector Research (ISTR) Istanbul, Turkey July 7-10, 2010


text:
Adria Watson
Adria is a junior at Sacramento State University where she is majoring in journalism. She has written and served as co-news editor for The State Hornet and freelanced for The Sacramento Bee. She comes to us through the Emma Bowen Foundation summer internship program, which CALmatters participates in.
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Susan Rubio, whose domestic violence allegations against her ex made headlines and cost him a seat in the Assembly, is a senator now. And she has a bill.
A black mother told not to scream in labor asks: Can California fix racism in maternity care?
Statewide as well as nationally, black women are substantially more likely than white women to suffer life-threatening complications during pregnancy, give birth prematurely, die in childbirth and lose their babies.

redpajama_set_name: RedPajamaCommonCrawl


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Parliamentary scrutiny of the British intelligence and security agencies
← Intelligence implications of Scottish independence
ISC Privacy & Security Inquiry – public sessions →
New Book – Watching the Watchers: Parliament and the Intelligence Services
Posted on October 9, 2014 by Andrew Defty
Our new book, Watching the Watchers: Parliament and the Intelligence Services, has now been published by Palgrave Macmillan.
The book provides a new and detailed examination of parliamentary scrutiny of the British intelligence and security agencies, and policy. Through detailed analysis of parliamentary business, coupled with interviews with more than 100 MPs and Peers and a number of senior officials in the Cabinet Office and the Foreign and Commonwealth Office, it examines the various mechanisms by which parliament seeks to scrutinise the secret state, and assesses the extent to which parliament has both the capacity and the will to provide effective oversight of intelligence and security policy and agencies. In addition to providing a detailed analysis of the impact of the Intelligence and Security Committee, this is the first book to examine the various other means by which a range of parliamentary bodies including select committees, all-party groups and individual parliamentarians have sought to scrutinise the intelligence agencies and the handling of intelligence by government.
Until recently, intelligence and security matters were not the subject of parliamentary debate in the United Kingdom. The veil of secrecy surrounding the intelligence and security agencies has gradually lifted since the late 1980s when a raft of legislation placed the agencies and their activities on a statutory footing. In particular, in 1994 the Intelligence Services Act created for the first time some form of parliamentary oversight of the intelligence and security agencies with the establishment of the Intelligence and Security Committee (ISC), a cross-party committee of parliamentarians, to examine the 'expenditure, administration and policy' of the agencies. Whilst the role of the ISC has expanded considerably since 1994, questions remain about whether this is the most effective means of providing oversight, and in 2013 the government introduced the first substantive reforms of the ISC as part of the Justice and Security Act.
There is also evidence of an appetite for greater parliamentary scrutiny of intelligence beyond the ISC. Prompted in part by the Labour government's use of intelligence to make the case for war in Iraq, terrorist attacks in the United Kingdom, and concerns about the role of the intelligence agencies in the interrogation of terrorist suspects, a number of parliamentary bodies and individual parliamentarians have pressed for broader parliamentary scrutiny of intelligence. In particular, in recent years a number of parliamentary select committees, most notably the Home and Foreign Affairs committees and the Joint Committee on Human Rights, have called for greater parliamentary accountability for the intelligence and security agencies, including the replacement of the ISC with a parliamentary select committee. In some areas All-Party Groups, such as the APG on Extraordinary Rendition, have sought to pressure the government and the ISC to reveal more about the work of the agencies. There is also evidence that the House of Lords is playing a more central role in the scrutiny of intelligence issues, with the first ever Lords debate on the work of the ISC in 2006, and the appointment of Peers with direct experience of the agencies, most notably Pauline Neville-Jones, former Chair of the Joint Intelligence Committee, and Eliza Manningham-Buller, the former Director-General of MI5, who used her maiden speech to attack proposals for the detention of terrorist suspects for up to 42 days.
Existing studies of parliamentary scrutiny of intelligence within the UK have focused almost exclusively on the work of the ISC. This is the first book to examine the role of parliament as a whole in this respect.
Chapter headings:
1. Introduction: The challenges of legislative oversight of intelligence
2. 'The Government does not comment': Parliament and the intelligence services
3. Managing continuity and change: legislating for intelligence agency accountability
4. 'A unique and special committee': the Intelligence and Security Committee
5. Issues of accountability and access: the select committees and intelligence
6. Other indicators of parliamentary interest: debates, questions, motions and groups
7. 'No longer scared to ask…': Parliamentarians and the intelligence services
8. New possibilities: legislative oversight of intelligence beyond Westminster
9. Conclusions: Parliament and the future of intelligence oversight
Sample chapter available on Palgrave website.
Hugh Bochel, Andrew Defty and Jane Kirkpatrick, Watching the Watchers: Parliament and the Intelligence Services, London: Palgrave Macmillan 2014, ISBN 9781137270429, hb. £68, also available as an Ebook.
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The 18th Judicial District Commission on Judicial Performance unanimously recommends that Judge Palmer L. Boyette BE RETAINED.
Judge Boyette became Magistrate for the Denver Juvenile Court in 2001 and was subsequently transferred to the Denver District Court, where he still serves part time as a Magistrate. In 2007, Judge Boyette was appointed to the bench and he now also serves part time in Elbert County. He graduated with a Bachelor of Arts in History from Florida State University in 1986. He graduated from Florida State Law School in 1989. Prior to his appointment, Judge Boyette worked as an Assistant City Attorney in Denver, and as a Senior Attorney in the Florida Department of Children and Families. He also worked in private practice and as an Assistant Public Defender in Naples Florida.
Judge Boyette is currently handling a diverse docket in Elbert County consisting of criminal, civil, misdemeanors, traffic infractions and small claims cases. He has received above average ratings from attorneys in many areas including application and knowledge of the law, issuing consistent sentences when circumstances are similar, treating participants with respect and setting reasonable schedules for cases. Although his marks from non-attorneys were slightly lower in these areas, his retention recommendation from this group was 82%. Due to the forgoing reasons, the Judicial Performance Commission unanimously recommends that Judge Palmer L. Boyette be retained.


This Aprils Fools lesson involving disgusting dead spiders (actually delicious gummy worms) shows how April fools relates to our faith. Some parts of our faith are tough to understand, like blood sacrifice and the crucifixion. Some unfortunate people can be fooled into thinking it's better to live without faith. But after we get close and trust just a little, we find our faith is delicious and fun…just like gummy worms!
Are you afraid to touch things that are kind of scary? Without looking? Get the student to say she isn't afraid.
Because, guess what? Today, my husband opened the bathroom closet. I screamed my fool head off! Guess what was in there, alive, and crawling around? Let them guess.
Probably 30 live disgusting spiders! My husband killed them all with the spray. I was scared. But it was my job to pick up all the dead spiders and put them in a plastic garbage bag.
One of them… run your fingers lightly up the blindfolded student's back and scratch at the back of her head… was still alive! I could see it wiggling and jiggling…it was so disgusting I almost screamed.
So! Guess what I brought into class today? (With sarcasm), Something I'm sure you'll all enjoy watching (blindfolded student's name) touch.
Put your finger to your lips and look at all watching students, so they will know that you are about to play a joke on her and not to give you away. Open the top of the Ziploc bag that the gummy worms are in. Make sure the student cannot see.
Go ahead (student's name). Touch what's in front of you. Tell us how it feels to touch it.
The student should be squeamish but finally touch. Maybe she will get what it is. Pull off the blindfold after a bit.
What was REALLY in the bag? Gummy worms.
APRIL FOOLS! Who would like some delicious candy gummies? Pass the bag around, allowing each child to take six.
It's April Fools Day. But I decided to play a trick on you so we can show you how our faith in Jesus contains a lot of April Fools.
Our faith is a lot like this bag of gummies. To hear some skeptical people talk, you'd think we had a bag of spiders.
Some people will say, "It's stupid to believe in a God. You can't see Him or hear Him. That's just plain dumb." All the while God is saying to them… Pick up a gummy worm and take a bite out of one yourself, smacking your lips.
Take another bite out of one gummy worm. Smack your lips!
Don't be April Fooled about God's rules! Try some out and see if you don't feel safer, more secure and more comforted with God in your life!
Take another bit out of the gummy worm. Smack your lips.
Christ's love every day we walk with Him!


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Blockchain is crucial for development, as it offers transformative solutions to tackle global problems, including climate change and world poverty. Despite the promising future, the technology itself is still far from mature. This, along with the unregulated nature of blockchain is making the Chinese government nervous. Despite assuring the people that China is prioritising blockchain and will support the technology to develop, the government is actually tightening their regulations, particularly on cryptocurrency.
China is a highly potential market for cryptocurrency, being a home to the world's biggest community of Bitcoin miners. However, in the past year alone, the country has passed a series of prohibiting regulations that have made it almost impossible for the cryptocurrency industry to thrive. Interestingly, some Chinese entrepreneurs see these strict regulations as an opportunity, and are trying to develop their businesses specifically to help the Chinese audience tap into the potential of investing in cryptocurrencies. Cointelegraph interviewed Yi Lu, one of the founders of media company SV Insight, and Xiahong Lin, founder of Blockchain prediction market platform Bodhi, to get their insights.


text:
\section{Introduction}

The current state of knowledge of planets around intermediate-mass
($M_\star \gtrsim 1.5$~M$_{\odot}$) stars is reminiscent of the general knowledge of
exoplanets in 2001. At that time there were 32 planets known, mostly
orbiting Sun-like stars. The distributions of semimajor axes and
masses ($M_P\sin i~$) of these early exoplanet discoveries, drawn from the
Exoplanet Orbit
Database\footnote{\tt{http://exoplanets.org}}, are shown in
Figure~\ref{fig:firstplanets}, illustrating the
prevalence of giant planets in unexpectedly close-in
orbits\footnote{While unexpected
  based on the sample of one provided by the Solar System, the
  existence of short-period Jovian planets was predicted in at least
  one published instance prior to the discovery of the first hot
  Jupiter \citep{mayor95}. In 1952 Otto Struve
  mused,  ``...[T]here seems to be no compelling reason
  why the...planets should not, in some instances,
  be much closer to their parent star than is the case in the solar
  system. It would be of interest to test whether there are any such
  objects.'' \citep{struve52}}. As of 2010 May there are 31 planets
known to orbit intermediate-mass stars ($M_\star > 1.5$~M$_{\odot}$), and the
semimajor axes of planets in this new class was surprising, but for a
different reason:
there are no planets orbiting closer than 0.6~AU
\citep{johnson07,sato08a}. As \citet{bowler10} showed,
the  planet populations orbiting host stars on either side of
1.5~M$_{\odot}$\ are distinct at the 4-$\sigma$ level.

Close-in, Jovian planets are
relatively easy to detect using radial velocities because of the larger
amplitude they induce and the increased number of orbit cycles per
observing time baseline. Their absence therefore cannot be due to an
observational bias given the large population of planets at longer
periods. Instead, it appears that
stellar mass has a dramatic effect on the
semimajor axis distribution of planets. However, it is not clear
whether this effect is a reflection of the process of planet formation
and migration, or instead related to the effects of the evolution of
the host stars.

Stellar evolution may be an important factor because Doppler surveys
of intermediate-mass stars are largely restricted to
post-main-sequence targets. While massive,
main-sequence stars are poor Doppler targets due to their rapid
rotation ($V_{\rm rot}\sin{i}$~$\gtrsim 50$~km~s$^{-1}$; \citet{lagrange09a}), their evolved
counterparts on the giant and subgiant branches are much slower
rotators ($V_{\rm rot}\sin{i}$~$\lesssim 5$~km~s$^{-1}$) and therefore have the narrow
absorption lines required for precise Doppler measurements. However,
as stars evolve their atmospheres expand and may encroach upon the
orbits of their planets. Simulations by \citet{nordhaus10},
\citet{carlberg09} and \citet{villaver09} have
suggested that the engulfment planets by the expanding
atmospheres of stars can account for the lack of close-in planets
around K-giants and clump-giants \citep[see
  also][]{sato08a}.

\begin{figure}[!t]
\epsscale{1.1}
\plotone{f1.eps}
\caption{The semimajor axes and minimum masses ($M_P\sin i~$) of the first
  32 Doppler-detected planets (gray circles). The majority of these
  planets orbit stars with $M_\star < 1.5$~M$_{\odot}$, and the planets span
  a wide range of semimajor axes. Also shown are the first 31
  Doppler-detected planets around massive stars ($M_\star >
  1.5$~M$_{\odot}$; open diamonds), and the sole hot Jupiter, HD\,102956\,b
  (filled five-point star). Compared to the population of planets
  around Sun-like  stars, there is a notable paucity of planets
  inward of 0.6~AU around the intermediate-mass
  stars.  \label{fig:firstplanets}}
\end{figure}

While Doppler surveys have encountered a barren region around A stars
inward of 0.6~AU, transit surveys have discovered two examples of hot
Jupiters around intermediate-mass stars. OGLE2-TR-L9 and WASP-33 are
1.5~M$_{\odot}$\ stars orbited by Jovian planets with semimajor axes $a =
0.041$~AU and 0.026~AU, respectively \citep{snellen09,
  cameron10}. These detections demonstrate
that close-in planets exist around A-type dwarfs,
adding additional concern that the lack of planets close to evolved
intermediate-mass stars is the result of stellar
engulfment. Unfortunately, the complicated observational and selection
biases inherent to ground-based, wide-field transit surveys make it
difficult to
measure accurate occurrence rates that can be meaningfully compared
to those measured from Doppler surveys \citep{gaudi05}.

Among the various types of evolved stars, subgiants offer a unique
view of the population of hot Jupiters around intermediate-mass
stars. The radii of subgiants have inflated by only a factor of $\approx
2$ compared to their main-sequence values. The simulations of
\citet{villaver09} show that planets with $a \gtrsim 0.1$~AU
should be safe from the tidal influence of stars near the base of the
RGB (see their Figure 2). It is only after stars start to ascend the
RGB and have their radii expand to an appreciable fraction of an AU
that tidal influences become important. The occurrence rates and
semimajor axis distribution of close-in planets around subgiants should
therefore be representative of the properties of planets around
A-type dwarfs.

We are conducting a Doppler survey of intermediate-mass subgiants at
Keck and Lick Observatories to study the effects of stellar mass on
the physical properties and orbital architectures of planetary
systems. Our survey has resulted in the detection
of 14 planets around 12 intermediate-mass ($M_\star \gtrsim
1.5$~M$_{\odot}$) stars, and 4 additional planets around less-massive
subgiants \citep[][Johnson et al. 2010b, submitted]{johnson06b,
  johnson07,johnson08b,bowler10, peek09, johnson10b}. In this Letter
we report the first Doppler-detected
planet within 0.6~AU of a ``retired'' (former) A star: a hot Jupiter
around a 1.68~M$_{\odot}$\ subgiant.

\section{Stellar Properties, Radial Velocities and Orbit}

HD\,102956\ (=HIP\,57820) is listed in the \emph{Hipparcos} Catalog with
$V=8.02$, $B-V = 0.971$, a
parallax--based distance of 126~pc, and an absolute
magnitude $M_V = 2.5$ \citep{hipp}.  Like most subgiants,
HD\,102956\ is chromospherically--quiet with an average $S = 0.17 \pm
0.02$ and  $\log{R^\prime_{HK}} = -5.09$ on the Mt. Wilson scale
\citep{wright04b}. We used the LTE spectral synthesis
described by \citet{valenti05} and \citet{fischer05b} to estimate the
spectroscopic properties. To constrain the low surface
gravities of the evolved stars we used the iterative scheme of
\citet{valenti09}, which ties the SME-derived value of $\log{g}$ to
the gravity inferred from the Yonsei-Yale  (Y$^2$) stellar models. Our
SME analysis gives  $T_{\rm eff} = 5054 \pm 44$~K,
$\rm [Fe/H] = +0.19 \pm 0.04$,
$\log{g} = 3.5 \pm 0.06$ and
$V_{\rm rot}\sin{i} = 0.30 \pm 0.5$~km~s$^{-1}$. We compared the star's
temperature, luminosity and metallicity to the Y$^2$ stellar model
grids to estimate a stellar mass
$M_\star = 1.68 \pm 0.11$~M$_{\odot}$\ and radius $R_\star =
4.4$~\plmn0.07~R$_{\odot}$. All of the stellar properties are summarized
in Table \ref{tab:starorbit}.

\begin{figure}[!t]
\epsscale{1.1}
\plotone{f2.eps}
\caption{Doppler measurements of HD\,102956\ from Keck Observatory phased
  at the orbital period of the planet. The error
  bars are the quadrature sum of the internal measurement uncertainties
  and 5~m~s$^{-1}$\ of jitter. The dashed line shows the best-fitting orbit
  solution of a single Keplerian orbit. The solution results in
  residuals with an rms scatter of 6.0~m~s$^{-1}$\ and
  $\sqrt{\chi^2_\nu}$~$=$~1.35, indicating a good fit to the data. \label{fig:orbit}}
\end{figure}

We began monitoring the radial velocity of HD\,102956\ in 2007 April and
we have gathered a total of 22\ measurements. After two seasons of
observing we noticed RV variability with an rms scatter of 41~m~s$^{-1}$,
which is much larger than the scatter predicted by the measurement
uncertainties and jitter levels typical of subgiants
\citep{fischer03, wright05, johnson10b}.
Table~\ref{tab:rv} lists our RV measurements, times of observation and
internal errors (without jitter). \citet{johnson10b} estimate a
typical jitter of 5~m~s$^{-1}$\ based on their analysis of 382
RV observations of 72 stable
subgiants observed at Keck with HIRES. We add this jitter
estimate in quadrature to the internal measurement errors to ensure
proper weighting of the data in our orbit analysis.

To search for the best-fitting orbit we used the partially-linearized
Keplerian fitting code
\texttt{RVLIN}\footnote{http://exoplanets.org/code/}
described by \citet{wrighthoward}. As an alternative to a periodogram
analysis, we first stepped through a grid of orbital
periods sampled from 1 to 100 days in 5000 equal,
logarithmically-spaced intervals. At each step we fixed
the period, searched for the best-fitting orbit and recorded the
resulting\footnote{We use $\sqrt{\chi^2_\nu}$\ to indicate the factor by which
the observed scatter about the best-fitting model differs from our
expectation based on the measurement errors. Thus, the
scatter about our model is a factor of 1.35\ larger than our
average error bar.} $\sqrt{\chi^2_\nu}$. We found a minimum ($\sqrt{\chi^2_\nu}$~$ = 1.15$) at periods near
6.5~days. The next
lowest minimum ($\sqrt{\chi^2_\nu}$~$ = 1.98$) occurs at $P = 3.47$~days. However,
with a best-fitting eccentricity of 0.95, the orbit solution is clearly
unphysical.

We then allowed the period to float in our {\tt RVLIN} analysis with
an initial guess of $P= 6.5$~days, and found that a single-planet
Keplerian model with a period $P =
6.4950 \pm 0.0004$~days, eccentricity $e = 0.048 \pm 0.027$ and velocity semiamplitude
$K = 73.7 \pm 1.9$~m~s$^{-1}$. The fit produces RV residuals with a
root-mean-squared (rms) scatter of 6.0~m~s$^{-1}$\ and reduced $\sqrt{\chi^2_\nu}$~$ =
1.35$, indicating an
acceptable fit. We used the false-alarm analysis of
\citet{howard09} to calculate FAP~$ < 0.001$ \citep[see
  also][]{johnson10a}. The resulting minimum
planet mass is $M_P\sin i~$~$=0.96$~M$_{\rm Jup}$, and the semimajor axis is $a =
0.081$~AU. The best-fitting solution is shown in Figure~\ref{fig:orbit},
where the plotted error bars are the quadrature sum of internal errors and
5~m~s$^{-1}$\ of jitter.

\begin{deluxetable}{lc}
\tablecaption{Stellar Properties and Orbital Solution for HD\,102956
\label{tab:starorbit}}
\tablewidth{0pt}
\tablehead{
\colhead{Parameter} & \colhead{Value}
}
\startdata
$V$   & $8.02 \pm 0.05$ \\
$B-V$ & $0.971 \pm 0.01$ \\
$Distance$ (pc) & $126 \pm 13$ \\
$M_V$ & $2.5 \pm 0.2$ \\
[Fe/H] & $+0.19 \pm 0.04$ \\
T$_{\rm eff}$ (K) & $5054 \pm 44$ \\
$V_{\rm rot}\sin{i}$~(km~s$^{-1}$) & $0.30 \pm 0.5$ \\
$\log{g}$    & $3.5 \pm 0.06$ \\
$M_\star$ (M$_{\odot}$) & $1.68 \pm 0.11$ \\
$R_\star$ (R$_{\odot}$) & $4.4 \pm 0.1$ \\
$L_\star$ (R$_{\odot}$) & $11.6 \pm 0.5$ \\
$\log R'_{HK}$  & $-5.09$ \\
Age (Gyr) & $2.3 \pm 0.5$ \\
 &  \\
$P$ (days) &  $6.4950 \pm 0.0004$ \\
$K$ (m\,s$^{-1}$) & $73.7 \pm 1.9$ \\
$e$ & $0.048 \pm 0.027$\\
$T_P$ (Julian Date) & $2455346 \pm 0.7$ \\
$\omega$ (degrees) & $12 \pm 40$ \\
$M_P\sin i~$\ (M$_{\rm Jup}$) & $0.96 \pm 0.05$ \\
$a$ (AU) & $0.081 \pm 0.002$ \\
$R_\star/a$ & $0.253 \pm 0.008$ \\
N$_{\rm obs}$ & 22 \\
rms (m\,s$^{-1}$) & 6.0 \\
$\sqrt{\chi^2_\nu}$ & 1.35 \\
\enddata
\end{deluxetable}

After identifying the best-fitting model, we use a Markov-Chain Monte
Carlo (MCMC) algorithm to
estimate the parameter uncertainties \citep[See,
  e.g.][]{ford05,winn07,bowler10}.  MCMC is a Bayesian inference
technique that uses the data to explore the shape of the likelihood
function for each parameter of an input model.  At each step, one
parameter is selected at random and altered by drawing a random variate
from a normal distribution. If the resulting $\chi^2$ (not reduced by
the number of free parameters $\nu$) value for the new
trial orbit is less than the previous $\chi^2$ value, then the trial
orbital parameters are added to the chain.  If not, then the
probability of adopting the new value is set by the difference in
$\chi^2$ from the previous and current trial steps.  If the
current trial is
rejected then the parameters from the previous step are adopted.
We adjusted the width of the normal distributions from which the steps
are drawn until we achieved a 30--40\% acceptance rate in each parameter.
The resulting ``chains'' of parameters form the posterior probability
distribution, from which we select the 15.9 and 84.1
percentile levels in the cumulative distributions as the ``one-sigma''
confidence limits. In most cases the posterior probability
distributions were approximately Gaussian. The orbital
parameters and their uncertainties are listed in
Table~\ref{tab:starorbit}.

As an additional check on the nature of the RV variations, we acquired
photometric observations of HD~102956 with the T3 0.4~m  automatic
photometric telescope (APT) at Fairborn Observatory.  A brief
description of the T3 data acquisition and reduction procedures, as
well  as the utility of the APT observations for eliminating false
positive detections, can be found in \citet{johnson10b}.

The APT collected two dozen observations in the Johnson $V$ and $B$
photometric bands between 2010 May 30 and June 23, near the end of the
2010 observing season.  The $V$ observations scatter about their mean with
a standard deviation of 0.0037 mag, consistent with T3's measurement
precision for a single observation \citep[e.g.,][Tables 2--3]{henry00c}.
A least-squares sine fit on the 6.4948-day radial velocity period yielded
a semi-amplitude of $0.0012\pm0.0010$ mag.  Identical results
were obtained for the $B$ observations. This tight upper limit to
photometric variability provides strong support for the planetary
interpretation of the radial velocity variations.

\section{The fraction of intermediate-mass stars with hot Jupiters}

Our Keck and Lick Doppler surveys of subgiant stars have time
baselines of 3 and 6 years, respectively, and the majority of the
target stars have more than 6 observations with jitter-limited
measurement precision ranging from 3--6~m~s$^{-1}$. Our precision, cadence
and time baseline provide us with the opportunity to assess the
fraction of intermediate-mass stars with hot Jupiters, which we define as
planets with $a < 0.1$~AU. This definition is somewhat arbitrary, but
it is consistent with definitions widely used by other studies of hot
Jupiters, which typically focus on Solar-mass stars and periods $P
\lesssim 10$~days. The most comprehensive study of this kind is that
of \citet{cumming08}, who measure an occurrence rate of $f = 0.004 \pm
0.003$ for $a < 0.1$~AU, $M_P\sin i~$~$\geq 1$~M$_{\rm Jup}$\ and primarily stars
with masses $M_\star < 1.4$~M$_{\odot}$. Their reported planet occurrence is
consistent with $f < 0.01$ at 95\% confidence.

Within our sample we restrict our analysis to stars with $M_\star >
1.45$~M$_{\odot}$\ (the evolved counterparts of A-type stars), $N_{\rm
  obs} > 3$, $V_{\rm rot}\sin{i}$~$ < 20$~km~s$^{-1}$\ and no evidence of double-lines
indicative of an SB2. Our sample
contains 137 stars that meet these
criteria. For each star we first perform a periodogram analysis and
use {\tt RVLIN} to search for orbit solutions near the strongest
periodicities using the same technique described by \citet{marcy05b}.
We then evaluate the FAP by estimating the
likelihood of improving $\chi^2_\nu$\ over that of a linear fit
\citep[see][for further details]{howard09}. For solutions with FAP~$ <
0.01$, we record the rms of the residuals about the best-fitting
orbit. For larger FAP values we record the rms about the best-fitting
linear fit to the RVs.

\begin{deluxetable}{lll}
\tablecaption{Radial Velocities for HD 102956\label{tab:rv}}
\tablewidth{0pt}
\tablehead{
\colhead{JD} &
\colhead{RV} &
\colhead{Uncertainty} \\
\colhead{-2440000} &
\colhead{(m~s$^{-1}$)} &
\colhead{(m~s$^{-1}$)}
}
\startdata
14216.805 &   11.40 &  1.18 \\
14429.150 &    5.77 &  1.39 \\
14866.114 &   37.10 &  1.30 \\
14986.851 &  -58.52 &  1.27 \\
15014.772 &   59.14 &  1.07 \\
15016.870 &  -49.20 &  1.13 \\
15284.917 &  -79.04 &  1.34 \\
15285.993 &  -14.32 &  1.25 \\
15313.915 &   43.48 &  1.25 \\
15314.828 &  -10.25 &  1.18 \\
15343.795 &  -66.93 &  1.17 \\
15344.885 &    3.98 &  1.35 \\
15350.786 &  -40.57 &  1.27 \\
15351.880 &   34.14 &  1.19 \\
15372.804 &   30.58 &  1.16 \\
15373.796 &  -42.13 &  1.22 \\
15374.753 &  -98.50 &  1.10 \\
15376.783 &  -28.67 &  1.12 \\
15377.812 &   30.78 &  1.10 \\
15378.749 &   50.22 &  1.12 \\
15379.787 &    0.00 &  1.13 \\
15380.805 &  -70.40 &  1.13
\\
\enddata
\end{deluxetable}

Next, we measure the largest velocity semiamplitude $K_{\rm up}$
that is consistent with the observed rms scatter for simulated planets
of various periods. Our method is
similar to that of \citet{lagrange09a} and \citet{bowler10}. For each
star we sample a range of orbital periods corresponding
to semimajor axes $0.04 \leq a \leq 0.10$~AU\footnote{The lower limit of
$0.04$~AU corresponds to  $a/R_\star = 2$ for a typical $M_\star =
1.7$~M$_{\odot}$\ subgiant with $R_\star = 4$~R$_{\odot}$, which is the smallest
scaled semimajor axis among the known hot Jupiters listed in the
Exoplanet Orbit Database.}. At each fixed period we generate a
sample of 3000 simulated orbits
with random phases and circular orbits sampled at the actual times of
observation. For each simulated orbit we also add 5~m~s$^{-1}$\ of random
noise to simulate jitter. We then record the
distribution of 3000 simulated velocity rms values and compare the
distribution to the rms of the measurements. Finally, we adjust $K$
until the measured rms is less than that of 99.7\% of the simulated
orbits, and record the semiamplitude as $K_{\rm up}$ at that period.

Repeating this procedure for all 137 stars provides a
measure the completeness of our survey for planets above a given
$M_P\sin i~$\ at each semimajor axis sampled in our simulations.
Figure~\ref{fig:complete} shows contours of constant completeness for
our sample, together with the position of HD\,102956,
demonstrating that we are 95\% complete for $M_P\sin i~$~$ > 1$~M$_{\rm Jup}$\ and $a
< 0.1$~AU.

Since each detection or nondetection of a hot Jupiter represents a
Bernoulli trial, the fraction of stars with planets in our sampled
range is given by the binomial distribution P$(f|k,N) \propto
f^k (1-f)^{N-k}$, where $N=137$ is the number of target stars
containing $k$ detections. For our sample we measure
an occurrence rate of $f = 1.2^{+1.2}_{-0.7}$, or $f < 0.034$ at 95\%
confidence for $M_P\sin i~$~$ \geq 0.9$~M$_{\rm Jup}$, which includes a single
detection, HD\,102956\,b with $M_P\sin i~$~$
= 0.96 \pm 0.05$. Restricting our analysis to planets more
massive than 1~M$_{\rm Jup}$\ we find $f < 0.025$  at 95\% confidence.

Based on their survey of main-sequence A-type stars,
\citet{lagrange09a} reported no planets with $P < 10$~days among a
sample of 50 stars\footnote{\citet{lagrange09a} do not report stellar
masses, but instead classify stars based on $B-V$ colors. We
selected stars from their Table 4 with colors $0.0 < B-V < 0.3$ as
representative of main-sequence A-stars in our mass range ($M_\star >
1.45$~M$_{\odot}$).}, or $f <
0.05$ at 95\% confidence. However, because their early-type stars are
such rapid rotators, their achievable velocity precision only allowed
them to rule out planets with $M_P\sin i~$~$ \gtrsim 8$~M$_{\rm Jup}$. Thus, our
estimate of the fraction of massive stars with hot Jupiters represents
a significant refinement compared to the previous
constraints. However, our sample size is still too small to provide a
meaningful comparison with the planet fraction measured by
\citet{cumming08} for less massive stars. An extension of our
subgiants survey to the Southern sky is therefore warranted, and is
currently underway at the Anglo Australian Observatory (R. Wittenmyer,
private communication). Additional constraints will be provided by the
\emph{Kepler} space-based transit survey \citep{kepler}.

\begin{figure}[!t]
\epsscale{1.2}
\plotone{f3.eps}
\caption{Detection limits of the Keck Doppler survey of
  intermediate-mass subgiants as a function of semimajor axis. The
  contours indicate the minimum
  planet mass detectable with a given fractional completeness, which
  is labeled to the left of each contour. The vertical dashed line
  shows the semimajor axis that is roughly equal to 2 stellar radii,
  assuming $R_\star = 4$~R$_{\odot}$, which is typical of stars in the Keck
  survey. The position of HD\,102956\,b is marked with a solid
  circle. \label{fig:complete}}
\end{figure}

\section{Summary}

We report the discovery of a hot
Jupiter ($e = 0.048 \pm 0.027$, $M_P\sin i~$~$ = 0.96$~M$_{\rm Jup}$, $P =
6.4950$~days) orbiting the
subgiant HD\,102956. At $M_\star = 1.68$~M$_{\odot}$, HD\,102956\ is the most
massive star known to harbor a
hot Jupiter, and this short-period system is the first detected as
part of a Doppler survey of evolved, intermediate-mass stars.

The existence of this planet demonstrates that the observed population
of close-in planets around subgiants is largely representative of the
``primordial'' planet population, in that close-in planets have not
been adversely affected by the relatively mild, post-main-sequence
expansion of their host stars. This aspect of subgiants, together with
their jitter-limited RV precision of $\approx 5$~m~s$^{-1}$, makes them
ideally suited for studying the properties of short-period planets
with a wide range of minimum masses around intermediate-mass stars.

Based
on our current stellar sample we estimate that
0.5--2.3\% of A-type stars harbor a planet with $a < 0.1$~AU and
$M_P\sin i~$~$ > 1$~M$_{\rm Jup}$, compared to the 0.4\% occurrence rate around
Sun-like stars \citep{cumming08}. While planets with $a < 1$~AU are
unusually rare around A
stars, it is possible that there exists a population of hot Jupiters
($a < 0.1$~AU) around intermediate-mass stars comparable to
what is found around Sun-like stars. If so, then the close-in desert
around A stars may simply be an exaggerated version of the ``period
valley''
observed around Sun-like stars, marked by a deficit of planets with
periods ranging from roughly 10--100 days, a sharp increase in the
number of detected planets beyond 1~AU, and a pile-up near $P=3$~day
\citep{udrysantos07, cumming08, wright09}. Doppler surveys of a
larger number of massive subgiants, together with careful analyses of
detections from transit surveys, will test this possibility.

\acknowledgments
We gratefully acknowledge the efforts and dedication
of the Keck Observatory staff, especially Grant Hill, Scott Dahm and
Hien Tran for their support of
HIRES and Greg Wirth for support of remote observing. We are also
grateful to the time assignment committees of NASA, NOAO, Caltech, and
the University of California for their generous allocations of
observing time. A.\,W.\,H.\ gratefully acknowledges support from a
Townes Post-doctoral Fellowship at the U.\,C.\ Berkeley Space Sciences
Laboratory. G.\,W.\,M.\ acknowledges NASA grant NNX06AH52G.
G.\,W.\,H acknowledges support from NASA, NSF,
Tennessee State University, and the State of Tennessee through its
Centers of Excellence program.
Finally, the authors wish to extend special thanks to those of
Hawaiian ancestry  on whose sacred mountain of Mauna Kea we are
privileged to be guests.
Without their generous hospitality, the Keck observations presented herein
would not have been possible.

redpajama_set_name: RedPajamaArXiv


text:
Home > where-to-go > la-libertad
Pyramids and Colonial Ambience
Temples, pyramids and cities of mud that survive inclement weather: Chan Chan, Huaca del Sol y la Luna, el Brujo are some of the most remarkable destinations in the province of La Libertad. It offers exquisite colonial architecture in the beautiful mansions that line its streets, living culture with deeply-rooted customs like fishing on Caballitos de Tortora (the traditional reed rafts of the northern coast), and renowned beaches that attract surfers from around the world.
It is the birthplace of the seductive "marinera", the national dance of Peru. La Libertad, the very picture of ancient nobility.
Location: North coast of Peru, beaches, fertile valleys, mountains and jungle.
Size: 25,962 Km2 (10,024 sq. miles)
more about La Libertad
Adventure, living culture and nature:
Archaeology buffs, birdwatchers, nature-lovers and surfers.
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Arid and semi-warm
Maximum temperature 28°C82°F Minimum temperature 14°C57°F
Regular flights from Lima to Trujillo City (45-50 minutes).
Lima-Trujillo: 560 Km on the Panamericana Norte highway(8 hours by car)
Distance from Trujillo City
Ascope (Ascope Province) 59 Km / 45 minutes Bolívar (Bolívar Province) 382 Km / 24 hours Chepén (Chepén Province) 131 Km / 2 hours 30 minutes Cascas (Gran Chimú Province) 103 Km / 1 hour 10 minutes Julcán (Julcán Province) 105 Km / 3 hours Otuzco (Otuzco Province) 75 Km / 2 hours San Pedro de Lloc (Pacasmayo Province) 82 Km / 1 hour 30 minutes Tayabamba (Pataz Province) 449 Km / 24 hours Huamachuco(Sánchez Carrión Province) 164 Km / 4 hours Santiago de Chuco (Santiago de Chuco Province) 170 Km / 5 hours 15 minutes Virú (Virú Province) 49 Km / 50 minutes
Lowest 3 masl (Salaverryl) Highest 4,008 masl (Quiruvilca)
How long to stay
Routes and Times
In two days, visitors can see the city. If you wish to visit the historic sites and enjoy nature, it is essential to stay 4 days.
Chan Chan Citadel 6.5 km / 16 minutes.
Huaca del Sol (Temple of the Sun) and Huaca de la Luna (Temple of the Moon) 8 km / 15 minutes.
Huacas de Moche (Moche Temples) Museum 7.8 km / 14 minutes.
Pakatnamú Complex 96 km / 2 hours .
Huanchaco Beach Resort 13.5 km / 22 minutes.
El Brujo Archaeological Complex 60 km / 1 hour 20 minutes.
Esmeralda Huaca 3.9 km / 10 minutes.
El Dragon (The Dragon) or Arco Iris (Rainbow) Huaca 5.4 km / 13 minutes.
Puerto Chicama or Puerto Malabrigo 70 km / 1 hour 15 minutes.
Cañoncillo Forest 120 km / 2 hours.
San Pedro de Lloc 82 km / 1 hour.
Pacasmayo Beach Resort 108 Km / 1 hour 30 minutes.
Markahuamachuco Archaeological Complex 185.5 Km / 4 hours.
Wiracochapampa 183 km
Cachicadán Hot Springs 182 Km / 4 hours.
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Trujillo Plaza Mayor (Main Square)
Visiting Hours : All day and night.
Location : City centre.
Martín de Astete established the plaza as the City centre under the orders of Diego de Almagro. The main part of the plaza...
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Martín de Astete established the plaza as the City centre under the orders of Diego de Almagro. The main part of the plaza contains the Freedom monument, a marble statue in the baroque style sculpted by the German artist Edmundo Müller.
Trujillo Cathedral
Visiting Hours : Daytime.
Location : Plaza Mayor
Built in 1666, the site holds valuable works of art, particularly canvasses from the Cuzco school and altarpieces.
Cathedral Museum
Visiting Hours : Mon - Fri 9.00 am - 1.00 pm and 4.00 pm - 7.
Location : Located in the side flank of Trujillo Cathedral.
It holds items linked to religion, carvings and paintings from the colonial period, which include the following two highlights: "La...
Visiting Hours : Mon - Fri 9.00 am - 1.00 pm and 4.00 pm - 7.00 pm/ Sat. 9.00 am - 1.00 pm.
It holds items linked to religion, carvings and paintings from the colonial period, which include the following two highlights: "La negación de San Pedro" (St Peter's Denial) and the portrait of St John the Baptist. The roof decorated with polychrome beams and the crypt with murals of the apostles give a unique character to the building.
Belén Church
Location : Crossroads of streets Almagro and Ayacucho.
Its construction began in 1680 and concluded in 1708. It was built with adobe, brick and straw. The entrance gateway is framed by two...
Its construction began in 1680 and concluded in 1708. It was built with adobe, brick and straw. The entrance gateway is framed by two towers with triangle pilasters. Inside, the arches, pilasters and pillars all portray the Trujillan tradition of the 17th century.
El Recreo Plazuela
Location : Jr. Pizarro, block 9.
The ancient plazuela (small plaza) indicates the road to the hills through its imposing gateway. Restored in 1986, the site contains the...
The ancient plazuela (small plaza) indicates the road to the hills through its imposing gateway. Restored in 1986, the site contains the ancient fountain that was originally discovered in the Plaza Mayor. The water deposit that fed the manor houses in the colonial era can be seen.
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Chan Chan Citadel (Trujillo)
Visiting Hours : Mon - Sun 9.00 am - 4.30 pm.
Location : 5 km north-west of Trujillo, in Moche valley...
The largest pre-Hispanic mud city in the Americas. Declared a World Heritage site by UNESCO in 1986. Chan Chan is thought to have been...
Location : 5 km north-west of Trujillo, in Moche valley (10 minutes by car).
The largest pre-Hispanic mud city in the Americas. Declared a World Heritage site by UNESCO in 1986. Chan Chan is thought to have been the capital of the Chimú kingdom, originally extending over more than 20 km2 from Huanchaco Port to the Campana hills. Archaeologists believe that it housed over 100,000 workshops, streets, walls and pyramid-shaped temples. Its massive walls are decorated with geometric figures, stylized animals and mythological creatures. The tour complements the visit to the Site's Museum.
Huaca del Sol (Temple of the Sun) and Huaca de la Luna (Temple of the Moon) (Trujillo)
Location : 8 km south of Trujillo city (15 minutes by car).
The Huaca del Sol (Temple of the Sun) served as a political – administrative centre and the Huaca de la Luna (Temple of the Moon) as a...
The Huaca del Sol (Temple of the Sun) served as a political – administrative centre and the Huaca de la Luna (Temple of the Moon) as a ceremonial centre. The Urban Zone is located between both, composed of houses, large avenues, allies, alleys and plazas, confirming the high levels of political, religious, economic and social organisation in the Moche culture. The Huaca de la Luna made of super-imposed temples resulting from the different stages of the Moche period. On some walls, beautiful polychrome murals can be observed, whose figures clearly depict the god Ai-apaec. Within the temple, archaeologists have discovered a tomb with over 40 sacrificed warriors. Tourist visits to the area currently only include the Huaca de la Luna.
Huacas de Moche (Moche Temples) Museum (Trujillo)
Location : 300 metros from the Huaca de la Luna (Temple of...
Inaugurated in June, 2010. Organized into three thematic halls, the structure refers to the building tradition of the Moche culture.
Location : 300 metros from the Huaca de la Luna (Temple of the Moon).
Huaca El Dragón (The Dragon's Temple) or Arco Iris (Rainbow Temple) (Trujillo)
Location : 4 km from Trujillo city (10 minutes by car).
An adobe pyramid, which is of great importance because its construction is believed to have occurred at the start of the Chimú culture...
An adobe pyramid, which is of great importance because its construction is believed to have occurred at the start of the Chimú culture and at the end of the Tiahuanco – Wari culture, between the 10th and 11th centuries. It is estimated to be 1,100 years-old. The building has a quadrangular shape and walls decorated with high relieves depicting zoomorphic and anthropomorphic figures. The name of the temple originates from one of said figures, a two-headed being with innumerable feet, similar to a dragon. Researchers believe that one of the roles of the site was ceremonial (potentially linked to rites in honour of the rainbow and other natural phenomena related to fertility).
Huanchaco Beach Resort (Trujillo)
Visiting Hours : Daytime and at night.
Location : 13 km north-west of Trujillo (15 minutes by car).
According to legend, Prince Tacaynamo landed in Huanchaco 800 years ago, founding the first Chimú dynasty. Its waters are still sailed by...
According to legend, Prince Tacaynamo landed in Huanchaco 800 years ago, founding the first Chimú dynasty. Its waters are still sailed by "caballitos de totora" (reed horses) traditional rafts used by fisherman on the north coast since the pre-Hispanic era. It is one of the favourite Peruvian beaches for surfing enthusiasts.
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Peru has become one of the world's most celebrated culinary destinations. Discover the incredible flavors of Peru.
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Gastronomy Expand ▼
Cebiche
Fish fillet cut into pieces cooked with lemon, onion and hot Limo chilies.
Sopa teóloga (Theologian's Soup)
Turkey and/or chicken soup with dipped bread, potatoes, milk and cheese.
Turkey pepián
Turkey stew with rice, ground sweet corn, coriander and chilies.
Shambar
Wheat soup made with pig skin and smoked ham, beans and spring onions. Served with toasted corn ('cancha'). Only available on Mondays.
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Festivals Expand ▼
Marinera Festival
The Concurso Nacional de Marinera (National Marinera Competition), one of the most elegant partner dances in Peru, is held at Trujillo's Gran Chimú...
Begins: 01-January-2015
The Concurso Nacional de Marinera (National Marinera Competition), one of the most elegant partner dances in Peru, is held at Trujillo's Gran Chimú Coliseum. Different categories and choreography styles are judged. Both dancers move while flapping a white shawl and making a series of characteristic steps. The man wears a poncho and a hat, as a paso horse rider, and the woman wears a beautiful, sensual outfit that is typical of the region. Location: Trujillo (34 masl).
Huanchaco Carnival
01 - 28 Feb
The Carnaval dates back to the beginning of the century, inspired in the Venetian Carnival. The tradition was updated 20 years ago and nowadays it...
Begins: 01-February-2014
Ends: 28-February-2014
The Carnaval dates back to the beginning of the century, inspired in the Venetian Carnival. The tradition was updated 20 years ago and nowadays it is celebrated with the election of the Carnival sovereign, allegorial carriage, krewes, people dressed in costumes, and contests.
Surfing Championship
It takes place in Malabrigo Beach (also known as Chicama), with surfers from all over the world taking part in this championship. This beach is...
Begins: 16-April-2014
Ends: 20-April-2014
It takes place in Malabrigo Beach (also known as Chicama), with surfers from all over the world taking part in this championship. This beach is famous worldwide for having the longest left-hand break in the world.
San José (Saint Joseph) Festival
Evokes Spanish traditions. Typical Spanish food and drinks are served, residents dress up, and the streets and houses are decorated in the Spanish...
Evokes Spanish traditions. Typical Spanish food and drinks are served, residents dress up, and the streets and houses are decorated in the Spanish style. There are processions of Peruvian Paso horses, a Pamplona-style bull run, bars and stages for Flamenco dances are assembled, and tunas (student music groups) take to the streets.
Virgin of the Gate
12 - 15 Dec
Mamita de la Puerta (Our Mother of the Gate) is known as the saint of the sick and disabled. Her departure from the church is a touching show: she...
Begins: 12-December-2015
Mamita de la Puerta (Our Mother of the Gate) is known as the saint of the sick and disabled. Her departure from the church is a touching show: she descends from high above the temple through an ingenious device to then be carried in procession. The image wears a long tunic studded with precious stones and is carried on a silver and precious metal crescent.
Contact Expand ▼
IPERÚ Trujillo Plaza de Armas
Jr. Independencia 467 – Of.106 – Plaza de Armas.
(044) 29-4561
iperutrujillo@promperu.gob.pe
L-S 9:00 – 18:00 horas/ D 9:00 – 13:00 horas.
IPERÚ Trujillo Complejo arqueológico Huaca de La Luna
Complejo Arqueológico Huaca de La Luna (Parador Turístico)
L-D 9:00 – 15:00 horas.
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text:
Зло́бичі — село в Україні, у Коростенському районі Житомирської області. Населення становить 362 особи.

Історія
У 1906 році — село Ушомирської волості Житомирського повіту Волинської губернії. Відстань від повітового міста 75 верст, від волості 15. Дворів 220, мешканців 1287.

У 1923—59 роках — адміністративний центр Злобицької сільської ради Коростенського району.

Примітки

Посилання
 Погода в селі Злобичі

Села Житомирської області

redpajama_set_name: RedPajamaWikipedia