text:
t is a strange mystery! The missing years refer to the period between Jesus' childhood and the commencing of his public ministry, curiously omitted from the New Testament record. He reappears later with the Gospel, good news. This message, where was it from? Was Christ a channel for Higher Intelligence? Was it the distillation of knowledge gained during this lost time? Maybe both. He is the logos, or Word of God. The man and this Eternal Word are inseparable, an even greater mystery.
We know little about the most famous man who ever lived. What we have is four books by four eye-witnesses. Matthew, Mark and Luke are the synoptic gospels, with John in a class by itself plus the Revelation. But what of the missing eighteen years between the ages of twelve and thirty? Not a word is mentioned about the most formative period in his development!
With trade routes, it seems hard to believe he never traveled at all but worked in carpentry, a trade of little use in his later life as an itinerant preacher. Why, if knowing he had but a short time in this world, would he not be at least curious to visit the great oriental mystery schools? The popular theory is that Jesus traveled extensively before returning to Judea and Galilee to begin his public ministry.
Mythos and Persona.
It is called the greatest story ever told. A legend larger than life: God Himself visiting the squalor of the earth as a man: Christ was kindhearted and sympathetic to the wretched suffering of those around him: Healing infirmity, the friend of sinners and outcasts: Giving absolution for mistakes made in life; compassionate and understanding of our flaws.
Truth Revealed to the Lowly.
In John Chapter 4. Jesus' dialogue with the Samaritan woman at Jacob's well is notable: First, it was a breach of social protocol for a Jewish rabbi to converse with a gentile woman- one of questionable reputation at that. Samaritans were considered mongrel Jews, but claimed the same Hebrew patriarchs as "our fathers who worshiped here at this mountain" (vs.12, 20). The disciples marveled at this, but said nothing. The Lord used the opportunity to say that the old ways had come to an end. "The time is coming, and already is, when God will be worshiped neither here at this mountain or at the temple in Jerusalem, but only in Spirit and in Truth." In a surprising move, she invokes the name of the messiah: The Christ to come. cf. 21-27. Then Jesus reveals to her his identity, "I am he."
Only by ritual blood sacrifices could one atone for sin, performed by the temple priests on certain festivals, requiring a pilgrimage for the people. The marble of the great shrine gleamed in the sunlight, standing proudly over Jerusalem as the very center of Judaism itself. Jesus stated that he was greater than the opulent temple. Sacrilege! Greater even than Abraham, the ancestral father of the Hebrews. The leaders were so appalled at this radical departure from tradition they accused the Lord of blasphemy.
Joshua bar Joseph was circumcised, b'rith milah, on the eighth day, according to the law. At age twelve, bar-mitzvah: The precocious lad astonished the elder rabbis in the temple for several days discussing the scriptures. Mary and Joseph thought he was lost, and a frantic search for the boy found him there. Luke 2:45-49. "Don't you know I must be about my father's business?"
The Family business not carpentry, but Architect of Life. We are left with only these words, Jesus increased in wisdom and stature, and in favor with God and man. The record falls silent before Jesus appears out of nowhere, a grown man of the age of thirty! cf. Matthew 2:27, 46-49; 3:13-17; Luke 2:52; 3:15; 23.
Coming to the Jordan River.
Among the crowds coming to John for baptism, he notices a man he instantly recognizes: The day he long awaited has arrived! He greets his cousin, and defers with humility- this is he! Christ the Lord. The harbinger reluctantly consents to baptize the only man who needed not repent of anything. As Jesus rose up from the waters, a Voice was heard from heaven... "This is my beloved Son in whom I am well pleased." Here is when the New Testament began.
Is this not Joseph's Son? (cf. Luke 4:16-28).
The young rabbi visits his hometown of Nazareth, attending the local synagogue. He is invited up to read. The scroll was handed to him. He opened to the prophet Isaiah, 61:1,2. All eyes were fixed on him as the congregation of men sat thinking, we recall this man since his youth, is this not Joseph's son? Jesus reads the ancient prediction, and implies he himself is the subject of Isaiah's prophecy of Israel's messiah to come.
"The Spirit of the Lord is upon me, he hath anointed me to preach good tidings unto the meek and the brokenhearted, the recovering of sight to the blind, liberty to the captives and deliverance to them that are bound. To proclaim the acceptable year of the Lord." He sits down again. There was silence before he drops the bombshell.
"Today this scripture is fulfilled in your ears!"
What did he say? How dare he! Knowing their thoughts, he chides them for their skepticism citing examples from scripture of the precious few in Israel who truly believed the prophets such as the widow of Sidon, and Naaman the Syrian, a gentile- the only leper cured in the Old Testament. It was an outrage!
Chased out by a mob, Jesus took his message elsewhere: Not one of Judaism or political revolt, but of a light within the soul of every man and a personal knowledge of the Living God: A kingdom already and not yet. "And they were astonished at his doctrine, for he spoke as one with authority, and not as the scribes." Jesus' words are impeccable, utterly irresistible. A message not of law but of grace. Not of punishment but forgiveness. Jesus understood we are only human beings, frail and weak of mind.
Judaism did not appear until after the return of Judah from Babylon. The captivity began in 586, BC, centuries after the Hebrew patriarchs, Abraham, Isaac, Jacob and Joseph. The Lord appeared as a Jew, the time was right, the empire was united under the Greek language and Hellenistic culture. Alexandria, not Jerusalem was the hub of Jewish thinking. The Romans built good roads for trade and travel along with a bustling maritime. Citizens were free to move about the world as they pleased.
The Jews had expected a great savior to free them from Roman occupation, but Jesus said first we must be saved from ourselves. The Son of David was not received by those of his own tribe, Judah, who still await their messiah. And Christians are watching for the Lord's return. Both are looking for a man to worship. The man Jesus did come, but Christ has never left.
I AM the Light of the World; I am the Way, the Truth and the Life; I am the Door; I am the Alpha and Omega; the Resurrection; the Good Shepherd; the True Manna; the Water of Life, etc.
Jesus the Water of Life - Powerful Scene from Ben-Hur
by kevinrspBelieves
Jesus' teachings were extemporaneous, he wrote nothing down that we are aware of. Only some words scrawled in the sand in defense of an adulteress-yet his beautiful Words have been preserved for us in red. Why red?
A rubric is a word or section of text that is traditionally printed in red ink for emphasis, often seen in missals. The word is derived from the Latin rubrica, meaning red ochre or chalk. This pigment requires a separate stage in the production of a manuscript.
Around 1900, rubrication was incorporated into the King James Version to distinguish the words spoken by Christ during his life because it lacked quotation marks. The gospel writer John said all the books in the world could not contain the things Jesus said and did. There must be more...
Other Sources Concerning the Missing Years.
1908, by Levi H. Dowling (1844-1911). "The Philosophic and Practical Basis of the Religion of the Aquarian Age."
"From the Akashic Records, the story of Jesus, the man from Galilee, how he attained the Christ consciousness open to all men. A record of the missing eighteen years, a period strangely silent in the New Testament; a period spent traveling and learning from the masters, seers and wise men in the temples and schools of Tibet, Egypt, India, Persia and Greece."
The title "Aquarian Gospel" comes from naming ages in terms of the dominant positions of constellations in the sky according to the earth's axial precession.
The 20th century marked the dispensation when this record would be revealed and understood, moving out of the former Age of Pisces (Christianity), to the Age of Aquarius (religious science).
The introduction describes the dramatic events in the heavens; the transition of Pisces, a water sign, to the age of Aquarius, an air sign seen in the inventions of aviation, radio, telegraph, etc.
What is an Age?
A terrestrial year is the movement of the earth around the sun, 365 days with four seasons. The sun moves through the elliptical, twelve tropical zodiac signs, equaling an Age, about 2,100 years. A sidereal year lasts for approximately 25,968 terrestrial years: The solar system revolves around a distant central sun in a 26,000-year precession of the equinoxes. It's a voyage of eons along the sidereal zodiacal belt. (2012 was expected to be a momentous sidereal year, a theory based on the Mayan calendar).
Ιησούς Χριστός. This book addresses the misunderstanding between the name of Jesus, and his title as the Christ: It doesn't refer to a Jewish messiah, or even a human at all, but the attainment of a high level of self-mastery or Christ Consciousness: A stage difficult to reach but open to every man. The Lord said, You marvel at my works. Greater things than these will you do!
The Aquarian Gospel has the ring of inspiration and truth, and to a degree satisfies the puzzle. Astounding clarity about the prehistoric origins of our ancestral religions. The mentoring of his cousin John, and Jesus' decision to leave for the orient with a traveler, a wealthy friend from India.
He meets with Brahmans, Buddhists, teaching on their errors. In Egypt, Jesus asks to be tested as an initiate and passes all seven of the difficult degrees. He is awarded the sign of circle seven. In Greece he explains how the Oracle at Delphi works. In every land he visited he was recognized as a master, and answered questions posed by the wisest men. He returns home to Galilee with the wisdom he distilled, the doctrines he shared with his own school of initiates:
All the elements in creation, from protoplast to plant, mineral, animal and man are on a long trek, evolving from being unaware to God-consciousness. After many incarnations the soul finally awakens, then continues to evolve over much time until it attains the Christ: It is to this end we are created.
The Urantia Book was published anonymously in 1955. It contains detailed records concerning life in the inhabited universe, the mechanisms of planetary hierarchies and the racial history of our own world, called "Urantia."
Over 2000 pages, with an exhaustive commentary on the life of Jesus Christ which almost defies comprehension. In this record he travels too, with the same friend from India he met in the Aquarian Gospel. He sails the Mediterranean world in order to better understand the gentiles; his intent is to reform Judaism with his gospel. Each year of his entire life is meticulously accounted for including exact dates. There are confusing details in this lengthy chronicle, detracting from the Christ we know in the Bible.
Avatar अवतार (Sanskrit) avatāra; a manifestation of deity in bodily form; an incarnate divine teacher. It relates his mission as an Avatar from the universe, attended to by a host of angels and other celestial intelligences who actually perform the wonders for him. In the early stages of his public ministry, Jesus seems unsure of himself, reticent as he struggles to come to terms with the ethical implications of the powers afforded him, and his destiny as the Son of God. The complexity of its cosmology makes for tedious reading and boggles the mind, beyond the scope of average understanding. We are left to wonder. The Urantia Book is quite an impressive work, well worth examining by the advanced student or anyone interested in learning more about the missing years of Jesus Christ.
In 1894 Nicolas Notovitch published a book called The Unknown Life of Christ. He was a Russian doctor who journeyed extensively throughout Afghanistan, India, and Tibet. Notovitch journeyed through the lovely passes of Bolan, over the Punjab, down into the arid rocky land of Ladakh, and into the majestic Vale of Kashmir of the Him-alayas. On one of his journeys he visited Leh, the capital of Ladakh, near the Buddhist convent Himis. He had an accident resulting in a broken leg, and stayed at the Himis convent. There he learned of the existence of ancient records of the life of Jesus Christ. In the course of his stay he was shown two large yellowed volumes containing the biography of St. Issa. Notovitch enlisted a member of his party to translate the Tibetan volumes, while he carefully noted in the pages of his journal over two hundred verses from the curious document known as "The Life of St. Issa."
When he returned to the western world, there was controversy as to the authenticity of the document. He was accused of creating a hoax and was ridiculed. In his defense he encouraged a scientific expedition to prove the original Tibetan documents existed.
One of his skeptics was Swami Abhedananda. Abhedananda journeyed into the arctic region of the Himalayas, determined to find a copy of the Himis manuscript or to expose the fraud. His book of travels, entitled Kashmir O Tibetti, tells visiting the Himis gonpa and includes a Bengali translation of two hundred twenty-four verses essentially the same as the Notovitch text. Abhedananda was thereby convinced of the authenticity of the Issa legend.
Oahspe (O-as-pee), is a channeled work published in 1882 by John Ballou. It contains the missing historical records regarding the origins of earth's major religions. The teachings of the great prophets and law-givers, Zarathustra of Persia, Brahma, Capilya and Sakaya of India, Abraham and Moses of Egypt, Joshu of Nazareth, Eawahtah of the Americas, and Po, Chine and Confucius of China.
Their teachings and doctrines are presented with a contemporary perspective on the New Age through spiritual progress. According to Oahspe (wisdom), all of humanity is responsible for assisting in its own development, and to that end it provides ample guidelines for ethical conduct in our day. The pages are divided to show the corresponding histories of the etherian realms above and the events of the corporeal world below. Oahspe has the ring of authority and Truth, a message for man in the modern century.
Copyright © 2018, The Pulpit
Hidden Spiritual Knowledge – Thepulpit.us
Hidden Spiritual Wisdom From The Bible – Thepulpit.us
Jesus, the "Missing Years."
Motion Pictures.
Pulpit Bible Study.
Religious Education – Thepulpit.us
Spiritual Knowledge – Thepulpit.us
Spiritual Lessons – Thepulpit.us
"Xanadu."


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redpajama_set_name: RedPajamaGithub


On August 3rd, you will be blamed for your own misfortunes. Your flaws may come out to bite you in the most painful way.
Do not be petty, do not be greedy, and do not lie - or at least try during this day. Ensure that you are not ruthless and you do not launch attacks on others for no reason. .
Day successful for acquisitions and efforts begun earlier with the real estate will be completed successfully. Ease of communication and business activity will prepare you for future labor week. But avoid to take on new responsibilities. Try to complete the important things and end long-standing disputes with relatives.
Day-friendly purification, release from addictions, attachments. Smokers Taurus will get a great chance to quit this addiction. Try today does not resort to using drugs, using the disease-fighting reserve forces of the organism and advice of traditional healers.
This day dedicate cultural activities. Visit exhibitions, museums, concert halls, theaters. These experiences create a reserve of spiritual forces for the next week. It is advisable to bring your children. Guests can visit relatives. Keep the doors open.
The day is associated with a weakening of the organism causing the disease, so we recommend a relaxing stay, employment and moderate exercise. As a result, you get the necessary margin of safety and health. Stars recommend these days to behave more relaxed than usual.
As a result, communication with children, you will understand their mistakes and miscalculations. You need to change, getting rid of excessive rigor and independence. It is possible that now begins a period that is associated with the ability to properly channel their vitality that will benefit the next week.
Active, creative day. Favorable for the people associated with art. Your rich inner world today may require non-traditional environment. A creative approach to business, full of feelings, personal attractiveness and kindness to others will bring substantial benefits.
Day of friendly meetings, intimate conversations and restore broken relationships. Perhaps in your life again will be a new man who was once able to see in you something that the other has not been revealed. His attention and participation will help you get rid of the doubt and will delight the soul.
This day can make many highly worrying and worrying. Today, there may well be serious changes in his personal life, associated with new acquaintances and break old ties. In any case, do not forget about those who have helped you in your life.
You may have a feeling of lethargy, fatigue. Excessive loads can you completely wear down. Slow down business activities, or may cause serious illness. You need a long rest.
Auspicious day for meetings, family celebrations, receptions. Your intuitive insight into the feelings of others, and the attractiveness of creative, original look at the things you will be able to arrange for others. But you have to stand up for their views. In the afternoon the possible health problems.
If you are looking for change, much can solve today, but the main results wait a little later. The likelihood of accidental acquaintances who do not remain without a trace in your life. During this period, you can improve your personal popularity and find love.


The goal of the MODRN project is to create cutting edge computer simulations of religious and social conflict in Norway, using modeling systems that enable "virtual" social experimentation by integrating empirically validated theories in the scientific study of religion (and secularization) within complex "causal architectures." These simulations will be calibrated using massive Norwegian datasets in dialogue with national and international experts in the fields of computer modeling, religious and secular diversification, and Norwegian public-policy.
MODRN will produce new tools for evaluating hypotheses about – and policies for – religious and socio-political change in Norway, Northern Europe and beyond. The three-year project began 1 July 2016 and runs through 30 June 2019. It is funded primarily by the Research Council of Norway, with additional funding from the University of Agder (UiA) in Kristiansand, Norway, the Institute for the Bio-Cultural Study of Religion (IBCSR) in Boston, Massachusetts, and the Virginia Modeling, Simulation and Analysis Center (VMASC) in Suffolk, Virginia, for a total budget of approximately 1.4 million USD.
The application of advanced strategies in computer simulation to the task of understanding the interrelation between micro- and macro-levels of social change will facilitate far more precise analysis (and creative synthesis) within academic and public discourse about the dynamics shaping religious conflict and secularization in an ecologically fragile, pluralistic and globalizing environment.


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Born 1952 in Tel-Aviv, Israel. Lives and works in Tel-Aviv.
1975-1978 Studies at Art Teachers' Training College, Ramat-Hasharon.
1986 -2007 Teacher of painting in the same institute (now Beit-Berl College School of Art).
Since 1982 Works with Givon Gallery, Tel-Aviv.


text:
\section{Introduction and Summary\label{sec:intro}}

\paragraph{Introduction} After a long journey, the Effective Field Theory of Large-Scale Structure (EFtofLSS) has been recently applied to the power spectrum of the galaxies of BOSS/SDSS~\cite{DAmico:2019fhj,Ivanov:2019pdj,Colas:2019ret}~\footnote{{Notice that Ref.~\cite{Colas:2019ret} is a companion paper to~\cite{DAmico:2019fhj}.} Ref.~\cite{DAmico:2019fhj} also applied it to the bispectrum, but finding marginal improvements, probably due to the fact that only the tree-level prediction was being used, so that the $k$-reach was not quite high.}. {These results have allowed us to measure all the cosmological parameters of the $\nu\Lambda$CDM model, except neutrino masses, just using a prior from Big Bang Nucleosynthesis (BBN).} The smallness of the error bars on some of these parameters have shown the power of Large-Scale Structure (LSS) surveys even without the inclusion of any cosmic microwave background (CMB) prior. For example, the constraint on the present-day dark matter fraction, $\Omega_m$, is competitive with the one from Planck2018~\cite{Aghanim:2018eyx}, and the one on the present-day Hubble parameter, $H_0$ is measured with the same precision as the one measured from Cosmic Distance Ladder, such as SH0ES~\cite{Riess:2019cxk}. Since the results from~\cite{DAmico:2019fhj,Ivanov:2019pdj,Colas:2019ret} are compatible with Planck, they contribute to shed light on the so-called Hubble tension (see a review in~\cite{Verde:2019ivm}). Though the number of modes in BOSS is much smaller than the ones in Planck, the origin of these remarkable results lies mainly in the fact that the CMB and LSS observables depend {quite} differently on the cosmological parameters, so that degeneracies are different (see for example sec.~4.3 of~\cite{DAmico:2019fhj}). Most importantly, these results show that the contribution of next generation LSS surveys, once analyzed with a controlled theory such as the EFTofLSS, to our  understanding of the history of the universe might be much larger than what previously believed, potentially helping to continue the remarkable exploration that was achieved in the past decades.

As mentioned, the application of the EFTofLSS to data is the result of a long journey where each of the ingredients of the EFTofLSS that was required in order to be able to apply it to data was one-by-one subsequently developed, tested on simulations, and shown to be successful. Though not all those intermediate results are directly used in the analysis, they were {\it necessary} for us, and probably for anybody else, to apply the model to data. We therefore find it fair, in each instance where the EFTofLSS is applied to data, to add the following footnote where we acknowledge at least a fraction of those most important developments~\footnote{The initial formulation of the EFTofLSS was performed in Eulerian space in~\cite{Baumann:2010tm,Carrasco:2012cv}, and subsequently extended to Lagrangian space in~\cite{Porto:2013qua}. The dark matter power spectrum has been computed at one-, two- and three-loop orders in~\cite{Carrasco:2012cv, Carrasco:2013sva, Carrasco:2013mua, Carroll:2013oxa, Senatore:2014via, Baldauf:2015zga, Foreman:2015lca, Baldauf:2015aha, Cataneo:2016suz, Lewandowski:2017kes,Konstandin:2019bay}. These calculations were accompanied by some  theoretical developments of the EFTofLSS, such as a careful understanding of renormalization~\cite{Carrasco:2012cv,Pajer:2013jj,Abolhasani:2015mra} (including rather-subtle aspects such as lattice-running~\cite{Carrasco:2012cv} and a better understanding of the velocity field~\cite{Carrasco:2013sva,Mercolli:2013bsa}), of the several ways for extracting the value of the counterterms from simulations~\cite{Carrasco:2012cv,McQuinn:2015tva}, and of the non-locality in time of the EFTofLSS~\cite{Carrasco:2013sva, Carroll:2013oxa,Senatore:2014eva}. These theoretical explorations also include an enlightening study in 1+1 dimensions~\cite{McQuinn:2015tva}. An IR-resummation of the long displacement fields had to be performed in order to reproduce the BAO peak, giving rise to the so-called IR-Resummed EFTofLSS~\cite{Senatore:2014vja,Baldauf:2015xfa,Senatore:2017pbn,Lewandowski:2018ywf,Blas:2016sfa}.  An account for baryonic effects was presented in~\cite{Lewandowski:2014rca}. The dark-matter bispectrum has been computed at one-loop in~\cite{Angulo:2014tfa, Baldauf:2014qfa}, the one-loop trispectrum in~\cite{Bertolini:2016bmt},
the displacement field in~\cite{Baldauf:2015tla}. The lensing power spectrum has been computed at two loops in~\cite{Foreman:2015uva}.  Biased tracers, such as halos and galaxies, have been studied in the context of the EFTofLSS in~\cite{ Senatore:2014eva, Mirbabayi:2014zca, Angulo:2015eqa, Fujita:2016dne, Perko:2016puo, Nadler:2017qto} (see also~\cite{McDonald:2009dh}), the halo and matter power spectra and bispectra (including all cross correlations) in~\cite{Senatore:2014eva, Angulo:2015eqa}. Redshift space distortions have been developed in~\cite{Senatore:2014vja, Lewandowski:2015ziq,Perko:2016puo}. Neutrinos has been included in the EFTofLSS in~\cite{Senatore:2017hyk,deBelsunce:2018xtd}, clustering dark energy in~\cite{Lewandowski:2016yce,Lewandowski:2017kes,Cusin:2017wjg,Bose:2018orj}, and primordial non-Gaussianities in~\cite{Angulo:2015eqa, Assassi:2015jqa, Assassi:2015fma, Bertolini:2015fya, Lewandowski:2015ziq, Bertolini:2016hxg}. Faster evaluation schemes for evaluation for some of the loop integrals have been developed in~\cite{Simonovic:2017mhp}.}.

\paragraph{Data sets} In this paper we focus on applying the EFTofLSS to analyze the $w$CDM model. We analyze various combinations among the full shape (FS) of BOSS DR12 pre-reconstructed power spectrum measurements  \cite{Gil-Marin:2015sqa}, baryon acoustic oscillations (BAO) of BOSS DR12 post-reconstructed power spectrum measurements \cite{Gil-Marin:2015nqa}, Planck2018 TT,TE,EE+lowE + lensing~\cite{Aghanim:2018eyx}. We also consider combinations with Supernovae (SN) measurements from the Pantheon Sample \cite{Scolnic:2017caz}. When quoting BAO, we also include measurements at small redshift from 6DF~\cite{Beutler:2011hx} and SDSS DR7 MGS \cite{Ross:2014qpa}, {as well as high redshift Lyman-$\alpha$ forest auto-correlation and cross-correlation with quasars from eBOSS DR14 measurements \cite{Agathe:2019vsu, Blomqvist:2019rah}.}
The inclusion of post-reconstructed BAO measurements gives a non-negligible improvement because the reconstruction amounts to using higher $n$-point functions. However the pre- and post-reconstruction BAO measurements are correlated. We describe how we account for this in App.~\ref{app:fsbao} {(see also~\cite{Philcox:2020vvt})}. When combined with Planck or SN, we simply add the {log-}likelihoods, since all the measurements refer to separate redshift bins. There is a small cross-correlation of the galaxy clustering data with the Planck weak lensing and the integrated Sachs-Wolfe (ISW) effect, which we neglect.

\paragraph{Methodology} The BOSS FS is analyzed following~\cite{DAmico:2019fhj,Colas:2019ret}.
The description of the theory model, as well as the likelihood analysis, including the covariances and priors used, can be found there.
Let us give a quick summary of our methodology.
The theory model is the galaxy power spectrum in redshift space at one loop in the EFTofLSS~\cite{Perko:2016puo, DAmico:2019fhj}.
The power spectrum is properly IR-resummed~\cite{Senatore:2014vja,Senatore:2017pbn,Lewandowski:2018ywf}, and includes observational systematics corrections: the Alcock-Paszynski effect~\cite{Alcock:1979mp}, window functions~\cite{Beutler:2018vpe}, and fiber collisions~\cite{Hahn:2016kiy}.
The EFT parameters are given physical priors as discussed in~\cite{DAmico:2019fhj}.
We sample over all $w$CDM parameters: the baryon abundance, $\omega_b$, the cold dark matter abundance, $\omega_{\rm cdm}$, the Hubble constant, $H_0$, the amplitude of the primordial fluctuations, $\ln (10^{10} A_s)$, the tilt of the primordial power spectrum, $n_s$, and the dark energy equation of state parameter, $w$, imposing no prior on the cosmological parameters but a BBN prior on $\omega_b$ (see main text for more details).

App.~\ref{app:fsbao} provides checks on the joint analysis of the FS with BAO, and App.~\ref{app:theoryerror} estimates the theoretical error of the model in $w$CDM: while the theory-systematic errors has been measured for $\Lambda$CDM in~\cite{DAmico:2019fhj,Colas:2019ret} using large-volume N-body simulations, and App.~\ref{app:theoryerror} presents an analogous measurement for the EFTofLSS on $w$CDM.

We find that BOSS pre-reconstructed and post-reconstructed data can be analyzed up to, respectively, $k_{\rm max } = 0.23 h\,{\rm Mpc}^{-1}$ and $k_{\rm max } = 0.3 h\,{\rm Mpc}^{-1}$, using the same model, likelihood, priors on EFT parameters, and corrections to observational effects as described in~\cite{DAmico:2019fhj}.
This is because we measure the theory-systematic errors in all cosmological parameters by fitting the simulations on $w$CDM with a BBN prior, and we find them to be negligible once compared to the error bars obtained in the various analyses presented in this paper.

\begin{figure}
\centering
\includegraphics[width=0.54\textwidth]{plots/wcdm_w-omega_m}
\caption{ \label{fig:wcdm_w-omega_m} $w-\Omega_m$ contour from the various analyses performed in this work. {When not analyzed in combination with CMB, we always use a BBN prior.} These results show the power of LSS, when analyzed with the EFTofLSS approach at long wavelengths, to constrain dark energy.}
\end{figure}

\paragraph{Main Results} The main results of our analysis are maybe best represented by Fig.~\ref{fig:wcdm_w-omega_m}. {Using late-time measurements only, FS+BAO+SN, but with a BBN prior on the baryons abundance, we obtain a tight bound: $w=-1.046_{-0.052}^{+0.055}$ at $68\%$ C.L. This is looser than, but nevertheless competitive with, Planck2018~\cite{Aghanim:2018eyx} combined with other probes. Additionally, our limits appear to be an improvement with respect to DES results when not using CMB information~\cite{Abbott:2017wau,Abbott:2018wzc}, though it is difficult to perform a precise and quantitative comparison in this case due to different combinations of external data sets and priors being used.  It is hard to make a direct comparison with former BOSS analyses~\cite{Alam:2016hwk} as well, because in this case their results are presented always in combination with Planck.
All products, plots, confidence intervals, results, etc., of our analyses are shown in sec.~\ref{sec:results}, and physical explanations on how all parameters from $w$CDM (but in fact several extensions of $\Lambda$CDM) can be measured independently using FS+BAO are discussed in sec.~\ref{sec:physics}.  Fitting the combination of all datasets, we obtain: $w=-1.023_{-0.030}^{+0.033}$.}

In our analysis, we have assumed that the BOSS data do not contain any residual systematic error. Given the additional cosmological information that the EFTofLSS enables us to exploit from these data, it might be important to investigate if potential undetected systematic errors can affect our results. We leave such investigation to future work.

\paragraph{Public Fast Code} Details on the code used to fit the FS, called PyBird: Python code for Biased tracers in redshift space, are given in sec.~\ref{sec:pybird}. In fact, an additional result of this paper is making available to the general community a fast and simple python-based code to perform the FS analysis of the power spectrum using the EFTofLSS.  Pybird can be found at \href{https://github.com/pierrexyz/pybird}{https://github.com/pierrexyz/pybird}, {where we also provide an explicit likelihood to be used in the MonteCarlo sampler MontePython~\cite{Brinckmann:2018cvx, Audren:2012wb}}.

\section{Results on $w$CDM}
\label{sec:results}

\subsection{FS + BAO (+ SN)}
Here we present our results on the CMB-independent analysis of the $w$CDM model with fixed neutrino masses.
The datasets we use are the following:
\begin{itemize}
    \item{FS} refers to the combination of the power spectra (monopole and quadrupole) of the three different sky-cuts CMASS NGC, CMASS SGC and LOWZ NGC.
    These are at the effective redshift $z_{\rm eff} = 0.57$ for CMASS and $z_{\rm eff} = 0.32$ for LOWZ, and the maximum wavenumber we consider is $k_{\rm max} = 0.23 h/{\rm Mpc}$ for CMASS and $k_{\rm max} = 0.20 h/{\rm Mpc}$ for LOWZ.  Ref.~\cite{DAmico:2019fhj,Colas:2019ret} showed that in $\Lambda$CDM, with this choice of $k_{\rm max}$, the theoretical systematic error is negligible for this data set with the theoretical model that we use. More explanations on this analysis are given at the beginning of appendix~\ref{app:fsbao}.

    \item{FS+BAO} refers to the combination of the previous dataset with the $H r_s$ and $D_A / r_s$ parameters measured from the post-reconstructed power spectra corresponding to the same sky-cuts.
    We include the covariance among these datasets calculated as explained in appendix~\ref{app:fsbao}.
    In addition, we add `small-$z$' BAO measurements at redshift $z_{\rm eff} = 0.106$ from 6DF and $z_{\rm eff} = 0.15$ from SDSS DR7 MGS, {as well as Ly$\alpha$ BAO measurements including auto-correlation and cross-correlation with quasars from eBOSS at $z_{\rm eff} = 2.34$ and $z_{\rm eff} = 2.35$ respectively, based on the likelihood of \cite{Cuceu:2019for}.}
    All these redshift bins are uncorrelated with the redshift bins of FS+BAO.
    \item{FS+BAO+SN} refers to the combination of the previous dataset plus the Pantheon catalogue of high-redshift supernovae.
\end{itemize}

We use a Gaussian prior on $\omega_b$ motivated from BBN constraints centered on $0.02235$ with $\sigma_{\rm BBN} = 0.0005$, which is obtained by adding up the theory and statistic error of~\cite{Cooke:2017cwo}. The fit is done considering the Planck prescription of one single massive neutrino with mass $0.06$ eV as done in \cite{Aghanim:2018eyx}.
We assume Gaussian initial conditions, pure CDM with no WDM/HDM admixture, and a dark energy fluid component described by constant-in-time equation of state $p=w \rho$ and without perturbations.
This is the standard phenomenological dark energy model traditionally analyzed using LSS data and named $w$CDM (see e.g.~\cite{Alam:2016hwk,Abbott:2017wau,Abbott:2018wzc}).

The best fits, means and one-sigma intervals of the 1D posteriors are given in Table~\ref{tab:wcdm_lss}.
The triangle plots are shown in Fig.~\ref{fig:wcdm_lss}, while the $w-\Omega_m$ contour is shown in Fig.~\ref{fig:wcdm_w-omega_m}. {Following~\cite{DAmico:2019fhj}, we compare our analysis pipeline with simulations in App.~\ref{app:fsbao}, finding negligible theoretical systematic errors in $w$CDM.}

\begin{table}
\centering
\scriptsize
\begin{tabular}{|p{3cm}|p{2cm}|p{2cm}|}
 \hline
FS+BAO & best-fit & mean$\pm\sigma$  \\ \hline
$w_{0,fld }$ &$-1.085$ & $-1.101_{-0.11}^{+0.14}$ \\
$100~\omega_{b }$ &$2.229$ & $2.236_{-0.05}^{+0.051}$  \\
$\omega_{cdm }$ &$0.122$ & $0.1286_{-0.011}^{+0.009}$ \\
$H_0$ &$69.68$ & $70.53_{-2.9}^{+2.4}$  \\
$\ln\left(10^{10}A_{s }\right)$ &$2.791$ & $2.664_{-0.24}^{+0.22}$  \\
$n_{s }$ &$0.9447$ & $0.9071_{-0.056}^{+0.057}$  \\ \hline
$\Omega_{0,fld }$ &$0.7014$ & $0.695_{-0.017}^{+0.018}$  \\
$\sigma_8$ &$0.7368$ & $0.7062_{-0.057}^{+0.049}$ \\
\hline
 \end{tabular}
 \begin{tabular}{|p{3cm}|p{2cm}|p{2cm}|}
 \hline
FS+BAO+SN & best-fit & mean$\pm\sigma$ \\ \hline
$w_{0,fld }$ &$-1.031$ & $-1.046_{-0.052}^{+0.055}$  \\
$100~\omega_{b }$ &$2.235$ & $2.235_{-0.052}^{+0.051}$ \\
$\omega_{cdm }$ &$0.1218$ & $0.1273_{-0.011}^{+0.0088}$  \\
$H_0$ &$68.69$ & $69.52_{-1.7}^{+1.5}$ \\
$\ln\left(10^{10}A_{s }\right)$ &$2.777$ & $2.724_{-0.18}^{+0.19}$  \\
$n_{s }$ &$0.9273$ & $0.9144_{-0.053}^{+0.055}$  \\ \hline
$\Omega_{0,fld }$ &$0.6931$ & $0.6892_{-0.011}^{+0.012}$\\
$\sigma_8$ &$0.7144$ & $0.7155_{-0.051}^{+0.045}$  \\
\hline
 \end{tabular} \\
\begin{tabular}{|p{3cm}|p{2cm}|p{2cm}|}
 \hline
FS+BAO {\tiny w/o Ly-$\alpha$}& best-fit & mean$\pm\sigma$ \\ \hline
$w_{0,fld }$ &$-1.021$ & $-1.109_{-0.15}^{+0.17}$  \\
$100~\omega_{b }$ &$2.236$ & $2.239_{-0.051}^{+0.051}$  \\
$\omega_{cdm }$ &$0.1298$ & $0.1439_{-0.019}^{+0.013}$  \\
$H_0$ &$69.2$ & $71.88_{-3.7}^{+2.9}$  \\
$\ln\left(10^{10}A_{s }\right)$ &$2.701$ & $2.537_{-0.27}^{+0.24}$  \\
$n_{s }$ &$0.9045$ & $0.8433_{-0.067}^{+0.082}$ \\ \hline
$\Omega_{0,fld }$ &$0.6809$ & $0.6769_{-0.021}^{+0.025}$ \\
$\sigma_8$ &$0.7087$ & $0.6918_{-0.057}^{+0.049}$ \\
\hline
\end{tabular}
\begin{tabular}{|p{3cm}|p{2cm}|p{2cm}|}
\hline
FS+BAO+SN {\tiny w/o Ly-$\alpha$}& best-fit & mean$\pm\sigma$  \\ \hline
$w_{0,fld }$ &$-1.077$ & $-1.083_{-0.056}^{+0.07}$ \\
$100~\omega_{b }$ &$2.247$ & $2.238_{-0.05}^{+0.052}$  \\
$\omega_{cdm }$ &$0.1405$ & $0.1434_{-0.019}^{+0.012}$  \\
$H_0$ &$71.28$ & $71.44_{-2.5}^{+1.8}$  \\
$\ln\left(10^{10}A_{s }\right)$ &$2.656$ & $2.553_{-0.21}^{+0.2}$  \\
$n_{s }$ &$0.856$ & $0.845_{-0.061}^{+0.081}$  \\  \hline
$\Omega_{0,fld }$ &$0.6778$ & $0.6746_{-0.014}^{+0.017}$  \\
$\sigma_8$ &$0.7264$ & $0.6937_{-0.051}^{+0.043}$  \\
\hline
\end{tabular}\\
\caption{\label{tab:wcdm_lss} Results on $w$CDM fitting various combinations of FS with BAO and SN.}
\end{table}

\begin{figure}[h!]
\centering
\includegraphics[width=0.99\textwidth]{plots/wcdm_lss_triangle}
\caption{ \label{fig:wcdm_lss} Triangle plot of $w$CDM fitting various combinations of FS with BAO and SN.}
\end{figure}

For our constraints on $w$CDM, we only show the results for FS + BAO and FS + BAO + SN, since the FS dataset alone does not constrain $w$ {very well, as this} is subject to strong degeneracies. This is to be expected, as we analyze only two close redshift bins with $z_{\rm eff} = 0.32$ and $z_{\rm eff} = 0.57$.
When adding BAO, $w$ is constrained to { $w=-1.101 \pm 0.12$ at $68\%$ C.L. ($\pm 0.25$ at $95\%$ C.L.).}
Much of the improvement is coming from the addition of the small-$z$ bins with $z_{\rm eff} = 0.106$ from 6DF and $z_{\rm eff} = 0.15$ from SDSS DR7 MGS at which dark energy has strong effect on the background evolution, allowing to {further} break the degeneracies. {Adding Ly-$\alpha$ BAO breaks {even more the} degeneracies, as it adds one more redshift point deep into matter domination. These combinations of FS plus the various BAO are shown in Fig.~\ref{fig:wcdm_fs-allbao}, and more discussions can be found in sec.~\ref{sec:physics}.}

Although {the result from FS+BAO} does not set a very strong constraint on $w$, it is interesting in itself since it shows the ability to measure dark energy evolution using only late-time observables.
Notice that the limits on $w$ from the BOSS (+SDSS/6DF) data are stronger than the ones from Planck2018 (+ lensing) alone, which measures $w$ to $-1.57_{-0.33}^{+0.16}$ at $68\%$ C.L. ($_{-0.40}^{+0.50}$ at $95\%$ C.L.)~\cite{Aghanim:2018eyx}.

The ability to measure $w$ with FS+BAO is to be contrasted with the SN measurements, which require an external input (usually from the CMB) to achieve competitive precision, to break the degeneracy line in the plane $w-\Omega_m$.
The SN constraint on $w-\Omega_m$ comes from the fact that they provide a measurement of the luminosity distance $D_L(z)$.
We can estimate the scaling on parameters at the median redshift of the SN sample, getting $D_L(z=0.25) \sim \Omega_m^{-0.055} |w|^{0.1}$, as can be inferred from table.~\ref{tab:derivatives}.
This is to be contrasted with the positive correlation between $w$ and $\Omega_m$ given by the FS+BAO measurements, as discussed in sec.~\ref{sec:physics}.
Therefore, the combination FS+BAO+SN allows a much tighter constraint on {$w=-1.046_{-0.052}^{+0.055}$}.
This sets a competitive limit from late-time measurements alone, and it is consistent with previous analyses~\footnote{Notice that the change of the results after adding SN is statistically consistent, as shown in Table~\ref{tab:wcdm_lss} which includes the best fit values. Consistently, Fig.~\ref{fig:wcdm_w-omega_m} shows that there appears to be no statistical incompatibility between the data sets, also when, as we will do next, we add the CMB data.}.

For instance, combined Planck2018 and BAO gives $w = -1.038_{-0.048}^{+0.055}$~\cite{Aghanim:2018eyx}, while combined Planck2015 and SN yields $w = -1.026 \pm 0.041$~\cite{Scolnic:2017caz}.
This strongly suggests that additional data from future spectroscopic and photometric surveys will allow to constrain dark energy in an unprecedented way.

\begin{table}
\centering
\scriptsize
\begin{tabular}{|p{3cm}|p{2cm}|p{2cm}|}
\hline
CMB+BAO & best-fit & mean$\pm\sigma$ \\ \hline
$w_{0,fld }$ &$-1.035$ & $-1.045_{-0.051}^{+0.056}$ \\
$100~\omega_{b }$ &$2.24$ & $2.238_{-0.014}^{+0.014}$  \\
$\omega_{cdm }$ &$0.12$ & $0.12_{-0.0011}^{+0.0011}$ \\
$100*\theta_{s }$ &$1.042$ & $1.042_{-0.00029}^{+0.0003}$  \\
$\ln\left(10^{10}A_{s }\right)$ &$3.051$ & $3.047_{-0.015}^{+0.014}$ \\
$n_{s }$ &$0.9667$ & $0.9658_{-0.0041}^{+0.0039}$ \\
$\tau_{reio }$ &$0.05767$ & $0.05514_{-0.0078}^{+0.0073}$ \\  \hline
$z_{reio }$ &$8.021$ & $7.751_{-0.76}^{+0.76}$ \\
$\Omega_{0,fld }$ &$0.6951$ & $0.697_{-0.012}^{+0.012}$ \\
$YHe$ &$0.2479$ & $0.2478_{-6.1e-05}^{+6.1e-05}$ \\
$H_0$ &$68.49$ & $68.75_{-1.5}^{+1.3}$ \\
$\sigma_8$ &$0.8239$ & $0.8244_{-0.017}^{+0.016}$ \\
\hline
 \end{tabular}
 \begin{tabular}{|p{3cm}|p{2cm}|p{2cm}|}
 \hline
CMB+FS & best-fit & mean$\pm\sigma$ \\ \hline
$w_{0,fld }$ &$-1.027$ & $-1.029_{-0.056}^{+0.063}$  \\
$100~\omega_{b }$ &$2.241$ & $2.238_{-0.014}^{+0.014}$  \\
$\omega_{cdm }$ &$0.1199$ & $0.12_{-0.0011}^{+0.0011}$ \\
$100*\theta_{s }$ &$1.042$ & $1.042_{-0.00028}^{+0.00029}$  \\
$\ln\left(10^{10}A_{s }\right)$ &$3.047$ & $3.044_{-0.015}^{+0.014}$  \\
$n_{s }$ &$0.9648$ & $0.9656_{-0.004}^{+0.004}$  \\
$\tau_{reio }$ &$0.05567$ & $0.05385_{-0.0077}^{+0.0073}$ \\  \hline
$z_{reio }$ &$7.817$ & $7.623_{-0.75}^{+0.77}$  \\
$\Omega_{0,fld }$ &$0.6935$ & $0.6923_{-0.016}^{+0.016}$ \\
$YHe$ &$0.2479$ & $0.2478_{-6.1e-05}^{+6.1e-05}$  \\
$H_0$ &$68.3$ & $68.26_{-1.8}^{+1.6}$  \\
$\sigma_8$ &$0.819$ & $0.8189_{-0.018}^{+0.016}$ \\
\hline
 \end{tabular} \\
 \begin{tabular}{|p{3cm}|p{2cm}|p{2cm}|}
 \hline
CMB+FS+BAO & best-fit & mean$\pm\sigma$  \\ \hline
$w_{0,fld }$ &$-1.018$ & $-1.021_{-0.044}^{+0.049}$  \\
$100~\omega_{b }$ &$2.238$ & $2.24_{-0.014}^{+0.014}$ \\
$\omega_{cdm }$ &$0.1198$ & $0.1197_{-0.0011}^{+0.0011}$  \\
$100*\theta_{s }$ &$1.042$ & $1.042_{-0.00029}^{+0.00029}$ \\
$\ln\left(10^{10}A_{s }\right)$ &$3.038$ & $3.045_{-0.015}^{+0.014}$  \\
$n_{s }$ &$0.9654$ & $0.9664_{-0.0039}^{+0.004}$ \\
$\tau_{reio }$ &$0.0526$ & $0.05492_{-0.0077}^{+0.0072}$  \\   \hline
$z_{reio }$ &$7.509$ & $7.722_{-0.74}^{+0.76}$ \\
$\Omega_{0,fld }$ &$0.6909$ & $0.6926_{-0.011}^{+0.012}$  \\
$YHe$ &$0.2478$ & $0.2479_{-6e-05}^{+5.9e-05}$ \\
$H_0$ &$67.98$ & $68.18_{-1.3}^{+1.2}$ \\
$\sigma_8$ &$0.8126$ & $0.8162_{-0.015}^{+0.014}$  \\
\hline
 \end{tabular}
 \begin{tabular}{|p{3cm}|p{2cm}|p{2cm}|}
 \hline
{ CMB+FS+BAO+SN} & best-fit & mean$\pm\sigma$  \\ \hline
$w_{0,fld }$ &$-1.028$ & $-1.023_{-0.03}^{+0.033}$ \\
$100~\omega_{b }$ &$2.236$ & $2.24_{-0.014}^{+0.014}$  \\
$\omega_{cdm }$ &$0.1202$ & $0.1197_{-0.001}^{+0.0011}$ \\
$100*\theta_{s }$ &$1.042$ & $1.042_{-0.00029}^{+0.00029}$  \\
$\ln\left(10^{10}A_{s }\right)$ &$3.036$ & $3.045_{-0.015}^{+0.014}$ \\
$n_{s }$ &$0.9658$ & $0.9663_{-0.004}^{+0.0039}$  \\
$\tau_{reio }$ &$0.0507$ & $0.05464_{-0.0076}^{+0.0072}$  \\  \hline
$z_{reio }$ &$7.321$ & $7.694_{-0.73}^{+0.76}$ \\
$\Omega_{0,fld }$ &$0.6914$ & $0.6931_{-0.0078}^{+0.008}$  \\
$YHe$ &$0.2478$ & $0.2479_{-6e-05}^{+6e-05}$  \\
$H_0$ &$68.13$ & $68.22_{-0.86}^{+0.82}$  \\
$\sigma_8$ &$0.8161$ & $0.8168_{-0.011}^{+0.011}$ \\
\hline
 \end{tabular} \\

\caption{\label{tab:wcdm_cmb} Results on $w$CDM fitting different combinations of CBM with FS, BAO and SN.}
\end{table}

\begin{figure}[h]
\centering
\includegraphics[width=0.99\textwidth]{plots/wcdm_cmb_lss_triangle}
\caption{ \label{fig:wcdm_cmb} Triangle plot of $w$CDM fitting various combinations of CMB with FS, BAO and SN.}
\end{figure}

\subsection{Combined CMB and FS + BAO (+ SN)}
In order to get the tightest constraints possible on $w-\Omega_m$, we add the Planck2018 datasets to the FS, BAO and SN.
When adding Planck2018, we include the temperature, polarization and lensing likelihoods as provided by the Planck collaboration, {that we will refer as `CMB'}. As for the nuisance parameters, we only consider the `lite' configuration with one nuisance parameter, since we verified that it gives very similar results with respect to the full configuration.
{When combined to CMB, we do not include Lyman-$\alpha$ BAO to facilitate comparison with other analyses. We checked that including them does not change the results.}
The best-fits, means and one-sigma intervals of the 1D posteriors are given in Table~\ref{tab:wcdm_cmb}.
The triangle plots are shown in Fig.~\ref{fig:wcdm_cmb}, and the $w-\Omega_m$ contour is shown in Fig.~\ref{fig:wcdm_w-omega_m}.

The results we get on CMB + BAO are similar to the one of~\cite{Aghanim:2018eyx}.
Our CMB + BAO constraint is $w=-1.045_{-0.051}^{+0.056}$, while CMB + FS gives $w=-1.029_{-0.056}^{+0.063}$, a similar constraint with a slight shift towards $-1$.
As argued in \cite{Ivanov:2019hqk} for the $\Lambda$CDM model, the similar error bars for the CMB + BAO and CMB + FS analyses are a coincidence given the BOSS volume and the reconstruction algorithm used to measure the BAO parameters: it is expected that the FS information will supersede the BAO information in the next-generation experiments.
At this stage, we note that both the FS and the BAO information break the degeneracy in the $w-\Omega_m$ plane displayed by the Planck fit alone.
The combination of CMB + FS + BAO gives an even tighter constraint: $w=-1.021_{-0.044}^{+0.049}$, which is about a $15\%$ improvement on the error bar compared to CMB + BAO.
This shows that the FS does add information on top of the BAO, even when in combination with CMB.
Finally, adding SN provides $w=-1.021_{-0.030}^{+0.033}$, our tightest constraint.
This combination gives similar error bars as CMB+BAO+SN measurements, $w=-1.028 \pm 0.031$~\cite{Aghanim:2018eyx}, but a slight shift towards $-1$.

\section{Physical Considerations}
\label{sec:physics}

Let us now try to understand analytically how the data allow us to break the degeneracies and give constraints on $w$, following the discussion in~\cite{DAmico:2019fhj}, which, in turns, is similar to what done for the CMB in~\cite{Percival:2002gq}.

\begin{figure}[h]
\centering
\includegraphics[width=0.99\textwidth]{plots/wcdm_fs-allbao_triangle}
\caption{Triangle plot of $w$CDM fitting the FS in combination with various BAO: BOSS, BOSS+small-$z$ (SDSS DR7 MGS/6DF) and BOSS+small-$z$+Lyman-$\alpha$.}
\label{fig:wcdm_fs-allbao}
\end{figure}

First, we notice that changing $w$ does not impact the shape of the primordial power spectrum.
The only effects are the modifications of the linear growth function and of the angular diameter distance, which affects the angular scale under which the BAO peak is seen.

\begin{table}
    \scriptsize
    \centering
    \begin{tabular}{|l|c|c|c|c|c|c|c|c|}
    \hline
    & \multicolumn{3}{c|}{$\theta_{\rm LSS, \, \perp}$}
    & \multicolumn{3}{c|}{$\theta_{\rm LSS, \, \parallel}$}
    & \multicolumn{2}{c|}{$\theta_{\rm LSS, \, V}$} \\
    \hline
    &$z_{\rm CMASS}$ & $z_{\rm LOWZ}$ & $z_{\rm Ly-\alpha}$
    &$z_{\rm CMASS}$ & $z_{\rm LOWZ}$ & $z_{\rm Ly-\alpha}$
    &$z_{\rm 6dF}$ & $z_{\rm MGS}$ \\
    \hline
    $\omega_{m}$
    &$-0.14$ & $-0.19$ & $0.15$
    & $-0.027$ & $-0.12$ & $0.20$
    & $-0.23$ & $-0.21$ \\
    $h$
    &$0.77$ & $0.86$ & $0.45$
    & $0.54$ & $0.72$ & $0.84$
    & $0.94$ & $0.91$ \\
    $|w|$
    &$-0.17$ & $-0.12$ & $-0.19$
    & $-0.25$ & $-0.21$ & $-0.11$
    & $-0.065$ & $-0.087$ \\
    \hline
    \end{tabular}
    \begin{tabular}{|l|c|c|c|c|c|}
        \hline
        & \multicolumn{2}{c|}{$D$}
        & \multicolumn{2}{c|}{$f$}
        & $D_L$ \\
        \hline
        &$z_{\rm CMASS}$ & $z_{\rm LOWZ}$
        &$z_{\rm CMASS}$ & $z_{\rm LOWZ}$
        &$z=0.25$ \\
        \hline
        $\omega_{m}$
        & $-0.12$ & $-0.08$
        & $0.30$ & $0.40$
        & $-0.055$ \\
        $h$
        & $0.25$ & $0.16$
        & $-0.59$ & $-0.80$
        & $ -0.89$ \\
        $|w|$
        & $-0.063$ & $-0.028$
        & $0.29$ & $0.25$
        & $0.10$ \\
        \hline
        \end{tabular}
\caption{Logarithmic derivatives of different observables with respect to cosmological parameters.}
\label{tab:derivatives}
\end{table}

BAOs mainly measure the combination $\theta_{\rm LSS, \, V} = \left( \theta_{\rm LSS, \, \perp}^2 \theta_{\rm LSS, \, \parallel}\right)^\frac{1}{3}$, where $\theta_{\rm LSS, \, \perp}$ and $\theta_{\rm LSS, \, \parallel}$ are the contributions perpendicular and parallel to the line of sight, which can be disentangled from measuring separately the monopole and the quadrupole of the power spectrum {in the FS analysis, or from measuring the anisotropic BAO parameters}.
The angles are the following ratios of length scales:
\begin{equation}
    \theta_{\rm LSS, \, \perp} \simeq \frac{ r_d(z_{\rm CMB})}{D_A(z_{\rm LSS})} \, , \quad
    \theta_{\rm LSS,\, \parallel } \simeq \frac{ r_d(z_{\rm CMB})}{ c\, z_{\rm LSS}/H(z_{\rm LSS})} \, ,
\end{equation}
where $r_d(z_{\rm CMB})$ is the sound horizon at drag redshift, and $z_{LSS}$ is the mean redshift of the data sample.
Following~\cite{DAmico:2019fhj}, to understand the approximate parameter scaling, we  take the log derivatives around a fiducial cosmology ($\omega_m=0.147$, $h=0.7$, $w=-1$), shown in tab.~\ref{tab:derivatives} for several quantities of interest.

From the table, we can read the approximate degeneracy lines for CMASS, LOWZ, small-$z$ and Ly$\alpha$:
\begin{eqnarray}\nonumber
&&\theta_{\rm LSS, \, \perp}(z_{\rm CMASS}) \sim \(h \, \omega_m^{-0.18} |w|^{-0.22} \)^{0.77},\qquad \theta_{\rm LSS, \, \parallel}(z_{\rm CMASS}) \sim \(h \, \omega_m^{-0.05} |w|^{-0.47}\)^{0.54},\\  \nonumber
&&\theta_{\rm LSS, \, \perp}(z_{\rm LOWZ}) \sim \(h \, \omega_m^{-0.22} |w|^{-0.14}\)^{0.86}, \qquad\theta_{\rm LSS, \, \parallel}(z_{\rm LOWZ}) \sim \(h \, \omega_m^{-0.16} |w|^{-0.29}\)^{0.72}\ ,\\ \nonumber
&&\theta_{\rm LSS, \, V}(z_{\rm 6dF}) \sim \( h \, \omega_m^{-0.25} |w|^{-0.069}\)^{0.94},\qquad \theta_{\rm LSS, \, V}(z_{\rm MGS}) \sim \(h \, \omega_m^{-0.23} |w|^{-0.096}\)^{0.91}\ , \\
&&\theta_{\rm LSS, \, \parallel}(z_{{\rm Ly}\alpha}) \sim \(h \, \omega_m^{2.4} |w|^{-1.3}\)^{0.84},\qquad \theta_{\rm LSS, \, \perp}(z_{{\rm Ly}\alpha}) \sim \(h \, \omega_m^{0.33} |w|^{-0.42}\)^{0.45}\ .
\end{eqnarray}

The relative amplitude of the BAO wiggles with respect to the smooth part instead gives a measurement of $\sim \omega_m$.
This is quite intuitive as, unlike the wavelength, the amplitude of the oscillating part is not affected by projection effects, and therefore simply scales as the density of baryons and dark matter at the time of recombination, which, in the case of fixed $\omega_b$, simply scales as $\omega_m$ (see~\cite{Mukhanov:2003xr} for a very pedagogical review and derivation).

Let us now consider the broadband signal.
The linear power spectrum monopole and quadrupole give a measurement of $b_1^2 A_s^{(k_{\rm max })}$ and $b_1 f A_s^{(k_{\rm max })}$, where $f(z_{\rm CMASS}) \sim \Omega_m^{0.3} |w|^{0.29}$ and $f(z_{\rm LOWZ}) \sim \Omega_m^{0.4} |w|^{0.25}$, $f$ being the log-derivative of the linear growth function.
Here $A_s^{(k_{\rm max })}$ represents the amplitude of the linearly evolved power spectrum at the maximum wavenumber of our analysis, as this is where the signal peaks.
The broadband signal gives also a measurement of the linear growth function $D$ since the linear power spectrum scales as $D^2$, while the loop one scales as $D^4$.
However, the dependence on $w$ is quite weak, since $D(z_{\rm CMASS}) \sim \Omega_m^{-0.12} |w|^{-0.063}$ and $D(z_{\rm LOWZ}) \sim \Omega_m^{-0.08} |w|^{-0.028}$.

These estimates allow us, in principle, to solve for the cosmological parameters of the $w$CDM model when using only LSS data.
We determine $\omega_m$ from the amplitude of the BAO oscillations.
Then, the BAO angles, the quadrupole/monopole ratio and the amplitude of the broadband signal will give a measurement of $h$, $A_s$ and $w$ {(as well as of $b_1$)}.
However, using only the FS dataset there will be large error bars in the recovered parameters, given the low precision of the quadrupole spectra, and of the LOWZ measurements.
In particular, we find a large anticorrelation among $w$ and $h$, and a positive correlation between $w$ and $A_s$, as predicted by our simple analysis~\footnote{To understand the sign of the correlation, notice that $w$ is negative, and so to make it larger in absolute value, it will move towards more negative values.}.

When adding the precise BAO data from the post-reconstructed power spectra, we are able to partially break the degeneracies.
A big improvement comes from adding small-$z$ BAO measurements,  as we have additional data points to break the $h-w$ degeneracy (and the $w-A_s$ one as a consequence), getting the final constraints in fig.~\ref{fig:wcdm_fs-allbao}. {The shift in the posteriors when adding small-$z$ BAO is consistent with what we observe in our tests on simulations, see App.~\ref{app:fsbao}. }

When we add SN data, we get a measurement of the luminosity distance $D_L = (1+z)^2 D_A$.
In the absence of calibration of absolute luminosities, we cannot determine $h$ and one gets the approximate degeneracy line $D_L(z=0.25) \sim \Omega_m^{-0.055} |w|^{0.1}$.
This is an anticorrelation between $\Omega_m$ and $w$, apparent from fig.~\ref{fig:wcdm_w-omega_m}.
As we discussed, FS+BAO data give an anticorrelation between $h$ and $w$ since $\omega_m$ is determined.
Therefore, $w$ and $\Omega_m \sim \omega_m / h^2$ are positively correlated.
This explains the good constraints we get when we add the SN dataset to FS+BAO.

\begin{table}
\centering
\scriptsize

\begin{tabular}{|p{3cm}|p{2cm}|p{2cm}|}
 \hline
$w$CDM & best-fit & mean$\pm\sigma$  \\ \hline
$b_{1,{\rm CMASS \, NGC} }$ &$2.133$ & $2.434_{-0.34}^{+0.27}$  \\
$c_{2,{\rm CMASS \, NGC} }$ &$0.2843$ & $0.7325_{-1.1}^{+0.33}$ \\
$b_{1,{\rm CMASS \, SGC} }$ &$2.22$ & $2.492_{-0.32}^{+0.25}$  \\
$c_{2,{\rm CMASS \, SGC} }$ &$0.9084$ & $1.294_{-0.67}^{+0.57}$  \\
$b_{1,{\rm LOWZ \, NGC} }$ &$2.003$ & $2.242_{-0.26}^{+0.21}$  \\
$c_{2,{\rm LOWZ \, NGC} }$ &$0.7832$ & $1.283_{-0.77}^{+0.61}$ \\
\hline
 \end{tabular}
 \begin{tabular}{|p{3cm}|p{2cm}|p{2cm}|}
 \hline
 $\nu \Lambda$CDM & best-fit & mean$\pm\sigma$  \\ \hline
$b_{1,{\rm CMASS \, NGC} }$ &$2.049$ & $2.134_{-0.18}^{+0.16}$  \\
$c_{2,{\rm CMASS \, NGC} }$ &$0.4218$ & $0.8085_{-0.83}^{+0.28}$ \\
$b_{1,{\rm CMASS \, SGC} }$ &$2.143$ & $2.186_{-0.16}^{+0.15}$ \\
$c_{2,{\rm CMASS \, SGC} }$ &$1.172$ & $1.258_{-0.51}^{+0.47}$ \\
$b_{1,{\rm LOWZ \, NGC} }$ &$1.966$ & $2.019_{-0.15}^{+0.14}$  \\
$c_{2,{\rm LOWZ \, NGC} }$ &$0.9203$ & $1.273_{-0.58}^{+0.51}$ \\
\hline
 \end{tabular}
\caption{\label{tab:eft_param} EFT parameters fitting BOSS FS + BOSS BAO on $w$CDM and $\nu \Lambda$CDM}
\end{table}

We finish this section with a comment on the EFT parameters measured in our analysis.
Although our main focus in this paper is on constraining cosmological parameters in $w$CDM, the EFT parameters are also of interest as they are related to galaxy formation physics.
We show the 68\%-confidence intervals in Table~\ref{tab:eft_param} obtained fitting BOSS FS + BOSS BAO on $w$CDM, and on $\nu \Lambda$CDM for comparison.
Details on the fit on $\nu \Lambda$CDM can be found in App.~\ref{app:fsbao}.
Only the EFT parameters that are actually varied in the fit are shown, while the others, as they appear only linearly in the galaxy power spectrum, are marginalized at the level of the likelihood, as performed in~\cite{DAmico:2019fhj,Colas:2019ret}.
More details on the marginalization can be found in App.~\ref{app:marginalized}.
In Table~\ref{tab:eft_param}, we can see that the constraints on the EFT parameters are weaker in the fit on $w$CDM with respect to the one on $\nu \Lambda$CDM.
In particular, the error bar on $b_1$ roughly doubles.
This is expected from the discussion above on the broadband signal:
varying $w$ opens larger degeneracies in the amplitude parameters, including the linear galaxy bias~$b_1$.
Furthermore, the shift in $b_1$ going from $w$CDM to $\nu \Lambda$CDM is also consistent in direction and size with the correlation with $w$, that is found to be less than (but consistent with)~$-1$.
As the EFT parameters are clearly determined, this measurement could in principle allow us to learn on galaxy formation mechanisms. It would be interesting if a mapping between galaxy formation models and EFT parameters were to be performed.
Besides, given that the error bars on the EFT parameters are quite inflated in $w$CDM, doing this would also provide a good opportunity to use priors on the EFT parameters, motivated from simulations or more phenomenological models, in order to obtain more stringent constraints on the cosmological parameters.
We leave these avenues for future work.

\section{PyBird: Python code for Biased tracers in redshift space}
\label{sec:pybird}

PyBird is a code written in Python 3, designed for evaluating the multipoles of the power spectrum of biased tracers in redshift space.
In general, PyBird can evaluate the power spectrum of matter or biased tracers in real or redshift space.
The equations on which PyBird is based can be found in~\cite{Perko:2016puo, DAmico:2019fhj}.
The main technology used by the code is the FFTLog~\cite{Hamilton:1999uv}~\footnote{\href{https://jila.colorado.edu/~ajsh/FFTLog/index.html}{https://jila.colorado.edu/~ajsh/FFTLog/index.html}}, used to evaluate the one-loop power spectrum and the IR resummation, see sec.~\ref{sec:fastresum} for details.

PyBird is designed for a fast evaluation of the power spectra, and can be easily inserted in a data analysis pipeline.
In fact, it is a standalone tool whose input is the linear matter power spectrum which can be obtained from any Boltzmann code, such as \code{CAMB}~\cite{Howlett:2012mh} or \code{CLASS}~\cite{Blas:2011rf}.
The PyBird output can be used in a likelihood code which can be part of the routine of a standard MCMC sampler.
The design is modular and concise, such that parts of the code can be easily adapted to other case uses (e.g., power spectrum at two loops or bispectrum).

The code is public and available at: \href{https://github.com/pierrexyz/pybird}{https://github.com/pierrexyz/pybird}, and it depends on the numerical libraries NumPy~\cite{Numpy} and SciPy~\cite{2020SciPy-NMeth}.
We also provide an explicit integration in the MCMC sampler MontePython 3~\cite{Brinckmann:2018cvx}, as well as a Jupyter notebook containing examples to start with.

PyBird can be used in different ways.
The code can evaluate the power spectrum either given one set of EFT parameters, or independently of the EFT parameters.
If the former option is faster, the latter is useful for subsampling or partial marginalization over the EFT parameters, or to Taylor expand around a fiducial cosmology for efficient parameter exploration~\cite{Colas:2019ret}. {PyBird runs in less than a second on a laptop.}

PyBird consists of the following classes:
\begin{itemize}
\item \code{Bird}: Main class which contains the power spectrum and correlation function, given a cosmology and a set of EFT parameters.
\item \code{Nonlinear}: given a \code{Bird()} object, computes the one-loop power spectrum and one-loop correlation function.
\item \code{Resum}: given a \code{Bird()} object, performs the IR-resummation of the power spectrum.
\item \code{Projection}: given a \code{Bird()} object, applies geometrical effects on the power spectrum: Alcock-Paczynski effect, window functions, fiber collisions, binning.
\item \code{Common}: containing shared objects among the other classes, such as $k$-array, multipole decomposition, etc.
\end{itemize}

We performed extensive tests on PyBird numerics, with particular attention on the numerical stability of the FFTLog.
Especially, zero padding and window are implemented following~\cite{McEwen:2016fjn}.
All numerical parameters (e.g. number of points, boundaries or bias of the FFTLog's) are chosen such as, for a given value, we get the same power spectrum for that value multiplied or divided by 2, within $0.02\%$ for $l=0$, and $0.2\%$ for $l=2$, up to $k \sim 0.3$.
In the same spirit, the Taylor expansions in the IR-resummation are under control.

Notice finally that the particular implementation of the IR-resummation that we describe next allows for a simple modification of the code so that the dependence on $A_s$ can be factorized. Therefore, the sampling over~$A_s$ could be done extremely fast.

\subsection{Fast IR-resummation scheme}
\label{sec:fastresum}

The resummed power spectrum can be written as a sum of the nonresummed power spectrum plus IR-corrections. These IR-corrections can be efficiently evaluated using the FFTLog, which allows for a quick evaluation.
In this appendix, we derive the mathematical details of such implementation.

After a straightforward manipulations, the IR-resummation in redshift space for biased tracers up to the $N$-loop order reads~\cite{Senatore:2014vja, Lewandowski:2015ziq}:
\begin{align}
P^\ell(k)|_N & = \sum_{j=0}^N \sum_{\ell'}  4\pi (-i)^{\ell'} \int dq \, q^ 2 \, Q_{||N-j}^{\ell \ell'}(k,q) \, \xi^{\ell'}_j (q), \label{eq:resumConvol}\\
\xi^{\ell'}_j (q) & = i^{\ell'}  \int  \frac{dp\, p^2}{2\pi^2} P^{\ell'}_j(p)  \, j_{\ell'}(pq).
\end{align}
where $|_N$ denotes the resummed power spectrum up to order $N$ and $P^{\ell}_j(k)$ and $\xi^{\ell}_j (k)$ are the $j$-loop order piece of the Eulerian power spectrum and correlation function, respectively. $Q_{||N-j}^{\ell \ell'}(k,q)$ encodes the effects from the bulk displacements and is given by:
\begin{align}
Q_{||N-j}^{\ell \ell'}(k,q) & = \frac{2\ell+1}{2} \int_{-1}^{1}d\mu_k \,\frac{i^{\ell'}}{4 \pi} \int d^2 \hat{q} \, e^{-i\mathbf{q} \cdot \mathbf{k}} \, F||_{N-j}(\mathbf{k},\mathbf{q}) \mathcal{P}_\ell(\mu_k) \mathcal{P}_{\ell'}(\mu_q), \label{eq:resumQ}\\
F||_{N-j}(\mathbf{k},\mathbf{q}) & = T_{0,r}(\mathbf{k},\mathbf{q})\times T_{0,r}^{-1}||_{N-j}(\mathbf{k},\mathbf{q}), \nonumber\\
T_{0,r}(\mathbf{k},\mathbf{q}) & = \exp \left\lbrace -\frac{k^2}{2} \left[ \Xi_0(q) (1+2 f \mu_k^2 + f^2 \mu_k^2) + \Xi_2(q) \left( (\hat k \cdot \hat q)^2 + 2 f \mu_k \mu_q (\hat k \cdot \hat q) + f^2 \mu_k^2 \mu_q^2 \right) \right] \right\rbrace , \nonumber
\end{align}
where $\Xi_0(q)$ and $\Xi_2(q)$ are given by:
\begin{align}
\Xi_0(q) & = \frac{2}{3} \int \frac{dp}{2\pi^2} \, \exp \left(-\frac{p^2}{\Lambda_{\rm IR}^2} \right)  P_{11}(p) \, \left[1 - j_0(pq) - j_2(pq) \right],\\
\Xi_2(q) & = 2 \int \frac{dp}{2\pi^2}\, \exp \left( -\frac{p^2}{\Lambda_{\rm IR}^2} \right)  P_{11}(p) \, j_2(pq) .
\end{align}
By expanding the exponential {in $F||_{N-j}(\mathbf{k},\mathbf{q})$ in powers of $k^2$} and performing the angular integrals in Eq.~\eqref{eq:resumQ} \footnote{To perform the angular integrals, we follow the steps of \cite{Lewandowski:2015ziq}, but here expanding the whole argument of the exponential.}, the terms in Eq.~\eqref{eq:resumConvol} can be put in the form of:
\begin{equation}\label{eq:IRcorr}
4\pi (-i)^{\ell'} k^{2n} \, \mathcal{Q}_{||N-j}^{\ell \ell'}(n,\alpha) \, \int dq \, q^ 2 \,  \left[ \Xi_i(q) \right]^n   \xi_j^{\ell'}(q) \, j_{\alpha}(kq),
\end{equation}
where $n$ is the integer power controlling the expansion of the exponential, $j_{\alpha}$ is the $\alpha$-th order spherical Bessel function, $\left[ \Xi_i(q) \right]^n$ denotes a product of the form $\Xi_0(q) \times ...  \times \Xi_0(q) \times \Xi_2(q) \times ... \times \Xi_2(q)$ such that the total number of terms in the product is $n$, and $\mathcal{Q}_{||N-j}^{\ell \ell'}(n, \alpha)$ is a number that depends on $N-j$, $\ell$, $\ell'$, $n$, $\alpha$ (and $f$).
In particular, at lowest order $n=0$, one gets nothing but the nonresummed power spectrum.
The contributions to the integrand of Eq.~\eqref{eq:IRcorr} are shown in Fig.~\ref{fig:IRcorrections}.
\begin{figure}[h]
\centering
\includegraphics[width=0.55\textwidth]{plots/IRcorrections}
\includegraphics[width=0.44\textwidth]{plots/IRintegrand}
\caption{ \label{fig:IRcorrections} {\it Left}: Various contributions appearing in the leading IR-corrections, Eq.~\eqref{eq:IRcorr} with $n=1$, for the matter real-space power spectrum, with $k = 0.2$. $\Xi_0(q)$ or $\Xi_2(q)$ are essentially acting as lowcut and a bandpass filters around the BAO peak, respectively, making the BAO the only relevant information for the IR-resummation, while the broadband is mostly filtered out. This illustrates the physical fact that the IR-resummation only acts on the wiggly part of the power spectrum.
{\it Right}: Typical IR-correction integrand for the linear part (blue) and the one-loop (orange), at $k= 0.2$, of the form: $4\pi q^2 \xi_j(q) \, [ e^{-\frac{k^2}{3} \Xi_0(q)} - 1 ] \, j_0(kq)$.  While the broadband information is irrelevant, most of the signal in the integral will come from the BAO. }
\end{figure}

Thus, the resummed power spectrum is equal to the nonresummed power spectrum plus IR-corrections written as an expansion in powers of $k^2$ (starting at $k^2$):
\begin{equation}\label{eq:masterIRformula}
P^\ell(k)|_N = P^\ell(k) + \sum_{j=0}^N \sum_{\ell'} \sum_{n=1} \sum_{\alpha} 4\pi (-i)^{\ell'} k^{2n} \,\mathcal{Q}_{||N-j}^{\ell \ell'}(n, \alpha) \, \int dq \, q^ 2 \,  \left[ \Xi_i(q) \right]^n   \xi_j^{\ell'}(q) \, j_{\alpha}(kq) \, ,
\end{equation}
{where we remind that $n$ is the integer controlling the expansion in powers of $k^2$ of the exponential of the bulk displacements, running up to a sufficient order to achieve convergence of the expansion up to the highest $k$ mode of interest. The explicit expressions for $\mathcal{Q}_{||N-j}^{\ell \ell'}(n, \alpha)$ can be found in PyBird repo either in the main code or in the Mathematica notebook. }
Therefore, evaluating the resummed power spectrum boils down to evaluating one-dimensional integrals that can be performed using the FFTLog.
The loops of the (nonresummed) power spectrum and correlation function can be evaluated using the FFTLog, see e.g.~\cite{Simonovic:2017mhp, Lewandowski:2018ywf}.
Then, the IR-resummation consists simply in correcting the power spectrum with a set of spherical Bessel transforms that, once again, can be performed using the FFTLog.
In practice, we find that expanding up to $n=8$ is sufficient to achieve convergence up to $k\sim 0.3 h\,{\rm Mpc}^{-1}$ for both $\ell = 0, 2$, and keeping terms contributing only significantly\footnote{Precisely, we keep only the terms with one power in $k^2 \Xi_2(q)$ (see \cite{Lewandowski:2015ziq} for the validity of such approximation), and drop a few more terms that are found to be irrelevant.}, the IR-resummation can be achieved with about $30$ FFTLog's.
Notice that the spherical Bessel transforms in Eq.~\ref{eq:masterIRformula} all present well-localized compact integrands around the BAO scales, allowing to perform the FFTLog with a few points ($\sim \mathcal{O}(200)$) to achieve good accuracy.

Finally, as discussed in ~\cite{Senatore:2014vja, Lewandowski:2015ziq}, the dependence on the displacements is analytic, and therefore the IR-resummation will agree to perturbation theory once this one is performed to extremely high order. In practice, indeed, in our procedure we are Taylor expanding the IR-resummation, which is equivalent to including the part of the perturbative loop that would encode the effect of the long displacements. The fact that we go to order $n=8$ means that effectively we are doing an eight-loop calculation, but effectively keeping track only of the part that is relevant for the IR-resummation.

\section*{Acknowledgements}
We thank Florian Beutler and H\'ector Gil-Mar\'in for support with the BOSS data, and Emanuele Castorina for useful discussions.
LS and GDA are partially supported by Simons Foundation Origins of the Universe program (Modern Inflationary Cosmology collaboration) and LS by NSF award 1720397.
GDA and PZ thank the Theoretical Physics Group at CERN for hospitality during part of this work.
PZ thanks Fran\c{c}oise Papa for hospitality during completion of this work.
The linear power spectra were computed with the CLASS Boltzmann code~\cite{Blas_2011}~\footnote{ \href{http://class-code.net}{http://class-code.net}}.
The posteriors were sampled using MontePython cosmological parameter inference code~\cite{Brinckmann:2018cvx, Audren:2012wb}~\footnote{ \href{https://github.com/brinckmann/montepython\_public}{https://github.com/brinckmann/montepython\_public}}.
 Part of the analysis was performed on the Sherlock cluster at the Stanford University, for which we thank the support team, and part on the HPC (High Performance Computing) facility of the University of Parma, whose support team we thank.

redpajama_set_name: RedPajamaArXiv


Stolen from marcyjo: Answer the questions based on your current top 50 artists (as listed in your overall charts).
I heard his cover of the Spider-Man theme, which is TOTAL love. Then "Everything" sealed the deal.
"Grace Kelly". And while I like that song, it wasn't until "Big Girl, You Are Beautiful" that I fell. Hard.
Okay... hmm. I can't think of anything! I mostly like them for their stripped-down rock sound.
All of them? I guess... 6? Plus all of the side projecty things like Lost Dogs, but not the Cornerstone Live albums.
"Undecided" -- it's catchy but ultimately very sad.
Without a doubt, Motor Cycle.
A tie! "Skullcrusher Mountain" and "I Feel Fantastic."
"The World's Colombian Exposition" - even though no one else seems to like it when I try to share it... LOL.
Singing along to "Cologne, Cerrone, Houdini" with Ashlyn the first time she tried to sing it.
I get happy anytime I hear anything from It Won't Be Soon Before Long.
Never. I haven't seen anyone live for AGES.
Well, "Ana Ng," but of his solo work, it was "Illinois" from State Songs, because that's the first song on the album!
Oh no, the second album.
John Linnell. Though I love Flansy, I ultimately go for the cerebral stuff Linnell writes.
Learning about them from chickadilly!
Oh, heck. I can't choose... lessee, "Something" has the highest play count right now, "Come Together" second.
Heh. I've been in three live productions!
"Master of the House" from Les Miserables.
Circle Slide - one of the best albums ever made, IMHO.
Probably the first one I ever heard, Pictures in the Sky, which contains "Screendoor."
Never, but I can always hope!
It used to be "Momo no hanabira," but Ashlyn drove it into the ground! So now it's "Freinger."
Yet another one where I listened once and the sheer number of tracks bumped him high.
I guess it's Hybrid Theory, though I might like others better if I listened again.
ACK, how do I choose... "Ladies of the World" has the highest playcount, though.
The songs on Where's God When I'm Scared?
There was only ever ONE. And it's a classic.
"I Will Follow You Into the Dark" - though I ultimately don't agree with the worldview behind the lyrics.
Wow, that took a solid HOUR to do. But fun!
Well, can I help you try out any of them? Let me know!
Oh, my! I haven't thought about Newsboys in years! I LOVED that song! *sings* Isabelle is a belly dancer with a kleptomaniacs restraint..."
Oh, I just LOVE the Buffy musical. Dr. Horrible beats it in sheer awesome, but it's pretty darn close.
I love the Newsboys - did you see my comment to gapporin above? We've seen them 4-5 times live as well. Wait oops! It was on his entry: We actually have been following the Newsboys since their first album. They opened for Mylon and Broken Heart at a show we saw in Abilene in '89 or '90. But how far they've come!
Cool! I'll be on the lookout!


text:
Psychology and Behavior in Sport/Exercise (3)
Sport and Exercise Science/Kinesiology (67)
Social Studies in Sport and Physical Activity (2)
You are looking at 21 - 30 of 74 items for :
"sweat rate" x
Page:12345678
The Hydration Profile of Female Cricket Players during Competition
Karen Soo and Geraldine Naughton
This study investigated the hydration profile of high-performance female cricket players competing at a national tournament. The profile comprised hydration monitoring (n = 18) and a questionnaire (n = 20). Our objectives were to 1) advance the understanding of fluid losses in cricket sessions across a tournament and 2) assess the hydration knowledge and practices in female cricket players. Body mass before and after each game inning was recorded in order to estimate sweat rate, sweat loss, and percentage body-mass loss. Comparisons were made between groups categorized according to level of activity during each inning. When sweat rates were estimated according to actual activity time, results were in the range of those in other female team sports but less than results from male cricket players. A range of knowledge of hydration issues was also observed. This study supports the need for individualized hydration recommendations and provides direction for further hydration education in women's cricket.
In International Journal of Sport Nutrition and Exercise Metabolism Volume 17 (2007): Issue 1 (Feb 2007)
Zinc Loss in Sweat of Athletes Exercising in Hot and Neutral Temperatures
Kevin Tipton, Nancy R. Green, Emily M. Haymes and Mary Waller
Zinc (Zn) loss from sweat of 9 male and 9 female athletes exercising under hot (35°C, HE) and neutral (25°C, ME) conditions was examined. Subjects exercised at 50% VO2max on a cycle ergometer for 1 hr during each trial. Cell-free sweat samples were analyzed for Zn by atomic absorption spectro-photometry. There was a significant interaction of time, gender, and temperature for whole-body sweat rates (WBSR). WBSR for males were higher during both trials and at each time. WBSR from the second half of exercise were higher than those from the first half for both sexes and temperature conditions. Sweat Zn concentration was higher in the NE than in the HE, but when the sweat rates were included, the rate of Zn loss was no different between HE and NE. Zn concentration of the sweat for the first half of exercise was over twice that of the second half. Sweat Zn concentration of the men was no different than that of the women; however, due to greater sweat rate, men had significantly higher Zn losses. Although total Zn losses are estimated to be relatively low compared to the RDA. exercise at moderate intensities may increase surface Zn losses.
In International Journal of Sport Nutrition and Exercise Metabolism Volume 3 (1993): Issue 3 (Sep 1993)
Sweat Mineral-Element Responses during 7 h of Exercise-Heat Stress
Scott J. Montain, Samuel N. Cheuvront and Henry C. Lukaski
Uncertainty exists regarding the effect of sustained sweating on sweat mineral-element composition.
To determine the effect of multiple hours of exercise-heat stress on sweat mineral concentrations.
Seven heat-acclimated subjects (6 males, 1 female) completed 5 × 60 min of treadmill exercise (1.56 m/s, 2% grade) with 20 min rest between exercise periods in 2 weather conditions (27 °C, 40% relative humidity, 1 m/s and 35 °C, 30%, 1 m/s). Sweat was collected from a sweat-collection pouch attached to the upper back during exercise bouts 1, 3, and 5. Mineral elements were determined by using inductively coupled plasma-emission spectrography.
At 27 °C, sweat sodium (863 [563] µg/mL; mean [SD]), potassium (222 [48] µg/mL), calcium (16 [7]) µg/mL), magnesium (1265 [566] ng/mL), and copper (80 [56] ng/mL) remained similar to baseline over 7 h of exercise-heat stress, whereas sweat zinc declined 42–45% after the initial hour of exercise-heat stress (Ex1 = 655 [362], Ex3 = 382 [168], Ex5 = 355 [288] µg/mL, P < 0.05). Similar outcomes were observed for sweat zinc at 35 °C when sweat rates were higher. Sweat rate had no effect on sweat trace-element composition.
Sweat sodium, potassium, and calcium losses during multiple hours of sustained sweating can be predicted from initial sweat composition. Estimates of sweat zinc losses, however, will be overestimated if sweat zinc conservation is not accounted for in sweat zinc-loss estimates.
In International Journal of Sport Nutrition and Exercise Metabolism Volume 17 (2007): Issue 6 (Dec 2007)
Water and Salt Balance of Well-Trained Swimmers in Training
Ronald J. Maughan, Lisa A. Dargavel, Rachael Hares and Susan M. Shirreffs
This study investigated fluid and electrolyte balance in well-trained male and female swimmers during 2 training sessions. Participants were 17 nationally ranked swimmers measured during a period of intensive training. Sweat loss was assessed from changes in body mass after correction for fluid intake and urine collection. Sweat composition was measured from waterproof absorbent patches applied at 4 skin sites. Air and pool-water temperatures were 36 °C and 27.4 °C, respectively. Training lasted 105 min in each session. All measured variables were similar on the 2 testing days. Mean sweat-volume loss was 548 ± 243 ml, and mean sweat rate was 0.31 ± 0.1 L/hr. Mean fluid intake was 489 ± 270 ml. Mean body-mass loss was 0.10 ± 0.50 kg, equivalent to 0.1% ± 0.7% dehydration. Mean pretraining urine osmolality was 662 ± 222 mOsm/kg, which was negatively associated with both mean drink volume consumed (p = .044, r 2 = .244) and mean urine volume produced during training (p = .002, r 2 = .468). Mean sweat Na+, K+, and Cl− concentrations (mmol/L) were 43 ± 14, 4 ± 1, and 31± 9, respectively; values were not different between males and females and were not different between days except for a marginal difference in K+ concentration. The average swimmer remained hydrated during the session, and calculated sweat rates were similar to those in previous aquatic studies.
Assessment of Physical Demands and Fluid Balance in Elite Female Handball Players During a 6-Day Competitive Tournament
Brian Cunniffe, Carissa Fallan, Adora Yau, Gethin H. Evans and Marco Cardinale
Little data exists on drinking behavior, sweat loss, and exercise intensity across a competitive handball tournament in elite female athletes. Heart rate (HR), fluid balance and sweat electrolyte content were assessed on 17 international players across a 6-day tournament involving 5 games and 2 training sessions played indoors (23 ± 2 °C, 30 ± 2% relative humidity). Active play (effective) mean HR was 155 ± 14 bpm (80 ± 7.5% HRmax) with the majority of time (64%) spent exercising at intensities >80% HRmax. Mean (SD) sweat rates during games were 1.02 ± 0.07 L · h-1 and on 56% of occasions fluid intake matched or exceeded sweat loss. A significant relationship was observed between estimated sweat loss and fluid intake during exercise (r 2 = .121, p = .001). Mean sweat sodium concentration was 38 ± 10 mmol · L-1, with significant associations observed between player sweat rates and time spent exercising at intensities >90% HRmax (r 2 = .181, p = .001). Fluid and electrolyte loss appear to be work rate dependent in elite female handball players, whom appear well capable of replacing fluids lost within a tournament environment. Due to large between-athlete variations, a targeted approach may be warranted for certain players only.
The Heat Tolerance Test: An Efficient Screening Tool for Evaluating Susceptibility to Heat
Daniel S. Moran, Tomer Erlich and Yoram Epstein
Individuals in the population who are not able to sustain heat and whose body temperature will start rising earlier and at a higher rate than that of others, under the same conditions, are defined as "heat intolerant."
The applicability of the heat tolerance test (HTT) in identifying individuals' tolerance/intolerance to heat is presented.
HTT is performed according to the following protocol: 120 minutes exposure to 40°C and 40% relative humidity in a climatic chamber while walking on a treadmill, dressed in shorts and T-shirt, at a pace of 5 km/h and 2% elevation. Rectal temperature and heart rate are continuously monitored, and sweat rate is calculated.
Results and Conclusion:
The HTT that is based on controlled exposure to an exercise-heat stress is an applicable and an efficient tool in differentiating between a temporary and permanent state of heat susceptibility.
In Journal of Sport Rehabilitation Volume 16 (2007): Issue 3 (Jan 2007)
Fluid Balance and Sodium Losses During Indoor Tennis Match Play
Matthew J.E. Lott and Stuart D.R. Galloway
This study assessed fluid balance, sodium losses, and effort intensity during indoor tennis match play (17 ± 2 °C, 42% ± 9% relative humidity) over a mean match duration of 68.1 ± 12.8 min in 16 male tennis players. Ad libitum fluid intake was recorded throughout the match. Sweat loss from change in nude body mass; sweat electrolyte content from patches applied to the forearm, calf, and thigh, and back of each player; and electrolyte balance derived from sweat, urine, and daily food-intake analysis were measured. Effort intensity was assessed from on-court heart rate compared with data obtained during a maximal treadmill test. Sweat rate (M ± SD) was 1.1 ± 0.4 L/hr, and fluid-ingestion rate was 1.0 ± 0.6 L/hr (replacing 93% ± 47% of fluid lost), resulting in only a small mean loss in body mass of 0.15% ± 0.74%. Large interindividual variabilities in sweat rate (range 0.3–2.0 L/hr) and fluid intake (range 0.31–2.52 L/hr) were noted. Whole-body sweat sodium concentration was 38 ± 12 mmol/L, and total sodium losses during match play were 1.1 ± 0.4 g (range 0.5–1.8 g). Daily sodium intake was 2.8 ± 1.1 g. Indoor match play largely consisted of low-intensity exercise below ventilatory threshold (mean match heart rate was 138 ± 24 beats/min). This study shows that in moderate indoor temperature conditions players ingest sufficient fluid to replace sweat losses. However, the wide range in data obtained highlights the need for individualized fluid-replacement guidance.
Responses of Motor-Sport Athletes to V8 Supercar Racing in Hot Conditions
Matt B. Brearley and James P. Finn
Despite the thermal challenge of demanding workloads performed in high cabin temperatures while wearing heavy heat-retardant clothing, information on physiological responses to racing V8 Supercars in hot conditions is not readily available.
To describe the thermal, cardiovascular, and perceptual strain on V8 Supercar drivers competing in hot conditions.
Thermal strain was indicated by body-core temperature using an ingested thermosensitive pill. Cardiovascular strain was assessed from heart rate, hydration status, and sweat rate. Perceptual strain was estimated from self-rated thermal sensation, thermal discomfort (modified Gagge scales), perceived exertion (Borg scale), and perceptual strain index.
Prerace body-core temperatures were (mean ± SD) 37.7°C ± 0.4°C (range 37.0°C to 38.2°C), rising to 39.0°C ± 0.4°C (range 38.4°C to 39.7°C) postrace. Driver heart rates were >160 and >170 beats/min for 85.3% and 46.7% of racing, respectively. Sweat rates were 1.06 ± 0.12 L/h or 13.4 ± 1.2 mL · kg−1 · h−1, and postrace dehydration was 0.6% ± 0.6% of prerace body mass. Drivers rated thermal sensation as hot (10.3 ± 0.9), thermal discomfort as uncomfortable (3.1 ± 1.0), and perceived exertion as very hard to very, very hard (8.7 ± 1.7) after the races. Overall physiological and perceptual strain were 7.4 ± 1.0 and 7.1 ± 1.2, respectively.
Despite the use of cooling, V8 Supercar drivers endure thermal, cardiovascular, and perceptual strain during brief driving bouts in hot conditions.
In International Journal of Sports Physiology and Performance Volume 2 (2007): Issue 2 (Jan 2007)
Influence of Successive Badminton Matches on Muscle Strength, Power, and Body-Fluid Balance in Elite Players
Javier Abian-Vicen, Adrián Castanedo, Pablo Abian, Cristina Gonzalez-Millan, Juan José Salinero and Juan Del Coso
The aim was to analyze the influence of competitive round on muscle strength, body-fluid balance, and renal function in elite badminton players during a real competition. Body mass, jump height during a countermovement jump, handgrip force, and urine samples were obtained from 13 elite badminton players (6 men and 7 women) before and after the 2nd-round and quarterfinal matches of the national Spanish badminton championship. Sweat rate was determined by using prematch-to-postmatch body-mass change and by weighing individually labeled fluid bottles. Sweat rates were 1.04 ± 0.62 and 0.98 ± 0.43 L/h, while rehydration rate was 0.69 ± 0.26 and 0.91 ± 0.52 L/h for the 2nd round and quarterfinals, respectively. Thus, dehydration was 0.47% ± 1.03% after the 2nd round and 0.23% ± 0.43% after the quarterfinals. There were no differences in prematch-to-postmatch jump height, but jump height was reduced from 37.51 ± 8.83 cm after the 2nd-round game to 34.82 ± 7.37 cm after the quarterfinals (P < .05). No significant differences were found in handgrip force when comparing prepost matches or rounds, although there were significant differences between dominant and nondominant hands (P < .05). The succession of rounds caused the appearance of proteinuria, hematuria, glycosuria, and higher nitrite and ketone concentrations in urine. Rehydration patterns during a real badminton competition were effective to prevent dehydration. A badminton match did not affect jump height or handgrip force, but jump height was progressively reduced by the competitive round. Badminton players' renal responses reflected diminished renal flux due to the high-intensity nature of this racket sport.
Hydration during Exercise in Warm, Humid Conditions: Effect of a Caffeinated Sports Drink
Mindy L. Millard-Stafford, Kirk J. Cureton, Jonathan E. Wingo, Jennifer Trilk, Gordon L. Warren and Maxime Buyckx
Caffeine is regarded as a diuretic despite evidence that hydration is not impaired with habitual ingestion. The purpose of this study was to determine whether a caffeinated sports drink impairs fluid delivery and hydration during exercise in warm, humid conditions (28.5 °C, 60% relative humidity). Sixteen cyclists completed 3 trials: placebo (P), carbohydrate-electrolyte (CE), and caffeinated (195 mg/L) sports drink (CAF+CE). Subjects cycled for 120 min at 60–75%VO2max followed by 15 min of maximal-effort cycling. Heart rate and rectal temperature were similar until the final 15 min, when these responses and exercise intensity were higher with CAF+CE than with CE and P. Sweat rate, urine output, plasma-volume losses, serum electrolytes, and blood deuterium-oxide accumulation were not different. Serum osmolality was higher with CAF+CE vs. P but not CE. The authors conclude that CAF+CE appears as rapidly in blood as CE and maintains hydration and sustains cardiovascular and thermoregulatory function as well as CE during exercise in a warm, humid environment.
In International Journal of Sport Nutrition and Exercise Metabolism Volume 17 (2007): Issue 2 (Apr 2007)

redpajama_set_name: RedPajamaCommonCrawl