text:
General News • Top Trending • Tv Shows
On My Block Season 3 Rumours About Its Cancellation, Upcoming News, possibilities, Plot You Should know:
Saturday, 15 February 2020, 06:13 pm EST
Riya K
Netflix's youngster show arrangement On my Block is returning with season 3, and we are eager to see it. After all the dramatization and secret in past seasons, it would have been an absolute catastrophe on the off chance that we was unable to get another season. Be that as it may, don't stress, Netflix realizes how to deal with its watchers.
On My Block season 3 release date on Netflix:
It's hard to foresee when the show will return.
Yet, the two seasons one and two hit Netflix in mid-to-late March 2018 and 2019 individually, so we'd expect a similar this time around – March 2020 – particularly as those differences have now been settled and the show can completely push ahead.
On My Block season 3 cast: Who's returning know more:
Monse (Sierra Capri), Ruby (Jason Genao), Cesar (Diego Tinoco), Jasmine (Jessica Marie Garcia), Jamal (Brett Gray), Ruby's sibling Mario (Danny Ramirez), and Spooky (Julio Macias) have all had their individual stories left fully open, so we'd anticipate that them all should be back on our screens. Olivia, be that as it may, lamentably lost her life subsequent to being shot.
The entertainer who played her, Ronni Hawk, experienced harsh criticism from the show's fan base a year ago after various genius Donald Trump and hostile to weapon control tweets surfaced. She tweeted the accompanying articulations after the shooting at Marjory Stoneman Douglas High School in Parkland, Florida, in which 17 understudies and staff individuals were slaughtered, and 17 others harmed.
On My Block Season 3- Trailer:
There is no trailer yet. We can just anticipate that the trailer should be discharged a month prior discharging the season. So we need to hold up to that point.
On My Block Season 3- Storyline:
The last season left the fans at the edge of the slope. As Cesar, Ruby, Jamal, and Monse have all been stole. Additionally, Monse had chosen to leave school to go to contemplate in a live-in school. Also, there is folklore going about Roller world. Julio Macias (Spooky) likewise indicated that the kidnappings may be connected with Roller World. Hence season 3 will be following every one of these riddles and move towards responding to all the inquiries that we have as a primary concern.
Also Read When Is Gotham Season 6 Coming out ? Is There Any Confirmed News All You Need to Know
Better Call Saul Season 5 To be back on Netflix in February
Aquaman 2' features a Release Date But Fans Will need to Wait Several Years


If you haven't done so, we strongly encourage you to carefully read our brief on Full Spectrum Leadership, so that you can better understand what leadership attributes will be assessed and what implications the results might have on your leadership approach.
Choose one answer to each statement that you believe reflects reality, not desirable answers, so that the result is truly relevant for you.
At the end of the assessment, you will be asked to fill in your name, e-mail and role.
You actively promote ethical standards throughout your organisation.
You actively promote social responsibility throughout your organisation.
You are concerned about global issues and future generations.
You feel at ease with uncertainty.
You could describe yourself as compassionate, forgiving and you display humility.
You build mutually beneficial partnerships and strategic alliances across boundaries.
You actively mentor and coach subordinates.
You are active in the local community, creating relationships that promote goodwill.
You promote environmental awareness and stewardship.
Others see you as empathetic, intuitive and inclusive.
You develop and consistently communicate the company's vision and mission.
You develop and consistently communicate the company's espoused values.
You are a living example of values-based leadership. You walk the talk.
You build an environment of trust among direct reports that brings out the best in people.
You are creative, passionate, committed and generous.
You seek advice, build consensus and create a positive spirit.
You are very focused on continuous learning, continuous renewal and innovation.
You are actively engaged in your own personal development and you support the personal development of direct reports/colleagues.
You empower people to make decisions and resist the temptation to micro manage the work of others.
You are adaptable, courageous and enjoy challenges.
You use metrics in some form of balanced scorecard to measure and manage performance.
You display strong analytical skills in evaluating systems and processes.
You consistently evaluate risks before embarking on new ventures.
You think strategically and move quickly to capitalize on opportunities.
You promote order, efficiency, productivity, quality and excellence.
You regularly communicate both good news and bad news with all staff.
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You regularly acknowledge and praise direct reports and staff for a job well done.
You are easily accessible to direct reports and all key staff.
You are calm in the midst of chaos and decisive in the midst of danger.
You maintain long-term perspective while dealing with short-term issues and goals.
You create, manage and control budgets effectively.
You are appropriately cautious in complex situations.
You constantly seek to improve the health and safety of staff.


Day 3, morning - Bring all breakouts together and develop an action plan, which will likely includewhite papers, journal articles, and other engagement activities.
theoreticians, modelers, data scientists, informatics scientists, decision-makers, etc. Underrepresented groups, early career scientists and graduate students are strongly encouraged to participate.
To build community involvement and input, a series of Charrettes (interactive webinars) will take place over the upcoming months. Those interested in attending the workshop as well as other stakeholders are highly encouraged to attend. First charrette: Weds, November 8th, 9 am MST, mark your calendars.


text:
from django.conf.urls import url, include
from django.contrib import admin

from django.conf import settings
from django.conf.urls.static import static

from ui import views

urlpatterns = [
    url(r'^project/(?P<project>[\w-]+)', views.project_dashboard, name='project_dashboard'),
    url(r'^repo/(?P<repo>[\w-]+)', views.repo_dashboard, name='repo_dashboard'),
    url(r'^repo/(?P<repo>[\w-]+)/smells', views.smells, name='smells'),
    url(r'^leaderboard/', views.leaderboard, name='leaderboard'),
    url(r'^wall-0f-shame/', views.wall_of_shame, name='wall_of_shame'),
    url(r'^', views.dashboard, name='overview_dashboard'),
]

redpajama_set_name: RedPajamaGithub


text:
Q: Best way to animating wxDC paints I ask because in each painting exists a flicker effect. For example, I have a panel
panel = wx.Panel(self, -1)
panel.Bind(wx.EVT_PAINT, self.asd)
framesizer.Add(panel, flag=wx.EXPAND)

the callback is the asd function. Now I paint
dc = wx.PaintDC(panel)

[...] setting brush and misc

i = 10
for x in range(1, 100):
    i = i + x
    dc.Clear() # <- Look this... it's correct?
    dc.DrawRectangle(i,10,50,50)

A: What you need to learn are double-buffering techniques. Fortunately, someone has already written up some good information on the subject on the wxPython wiki:

*

*http://wiki.wxpython.org/DoubleBufferedDrawing
You will want to take a look at wx.BufferedPaintDC

redpajama_set_name: RedPajamaStackExchange


Please contact Pippa to check availability for both Monday classes before booking your try out class@£12.
WORKSHOP on Saturday FEBRUARY 2nd, 2019. Please go to workshop/retreats.
The Wednesday class is drop in only. No need to book. Please check availability before booking for both Monday classes, and contact Effraspace if you are interested in the class in SW2 which starts Sept 4th 2018.
Beginners and those with more experience are welcome to all classes. Equipment is provided at all venues.
You will need your own mat for the Well Woman class at Cufos, I do have a spare mat if you are trying out the class, but let me know.
Go round to the right hand side of the building to enter.
TRY OUT class £12. Check for availability before booking!
Drop in by arrangement only when space is available.
Free parking in neighbouring roads.
Venue is on the corner of Ribblesdale Rd, the map is not exact.
Please check for availability and then book a try out class using the button above.
to be taken any time within a 6/7 week block.
Some concessions are available on request.
Free parking at H. C. Club and in neighbouring roads.
Classes are ongoing and non bookable.
Venue is opposite the petrol station and Cooperative shop.
Restricted meter parking. Check carefully!


text:
A Baroque Bouquet
Debra Reuter-Pivetta
Greensboro -- ( Thu., Feb. 23, 2012 )
Greensboro Symphony Orchestra: Music by Bach, Handel, & Vivaldi
Performed by Dmitry Sitkovetsky, violin & conductor
$38, $32, $28, $22, students $5. -- War Memorial Auditorium , 336/335-5456, ext. 224 , http://www.greensborosymphony.org/ -- 7:30 PM
Greensboro -- ( Sat., Feb. 25, 2012 )
$38, $32, $28, $22, students $5. -- Dana Auditorium , 336/335-5456, ext. 224 , http://www.greensborosymphony.org/ -- 8:00 PM
By Timothy H. Lindeman
February 23, 2012 - Greensboro, NC:
The Greensboro Symphony Orchestra, led by Music Director Sitkovetsky, shed some weight Thursday night to fit into a guise of a much smaller Baroque orchestra, mostly strings, perfectly in keeping with performances by the giants of the first half of the 18th century — Bach, Handel and Vivaldi.
Bach wrote four orchestral suites, collections of stylized dances intended to be listened to, not danced. The GSO performed Suite No. 2 in B minor S. 1067, written for flute, strings and continuo. GSO first chair flutist Debra Reuter-Pivetta served as soloist, with Nancy Johnston at the harpsichord and Beth Vanderborgh on cello comprising the continuo.
The Overture begins with pompous, jerky rhythms, with first violins and flute doubling the melodic line. In the fast, imitative middle section, however, the flute breaks free and finds its own voice. Then begin the dances proper: Rondeau (a Gavotte), Sarabande, Bourrée, Polonaise, Menuet, etc. Each contrasts in character, tempo and mood, and each is in two parts, which were often repeated.
Some of the repeats featured new instrumentation, with the principal chairs acting as a string quartet with Reuter-Pivetta; this contrasting texture helped keep the piece fresh. In part of the Polonaise, only the flute and the continuo played, and each phrase ended with a big ritard — maybe not so stylistically correct, but certainly fun.
The finale movement, entitled "Badinerie" (which roughly translates "jesting") is a tour-de-force for the flute, sort of an encore to the whole proceedings. Throughout the work Reuter-Pivetta displayed a lovely tone, long winded lines, and often tasteful ornaments. Special kudos go to both Vanderborgh and Johnston who provided a solid base throughout the evening.
Handel's Water Music was written in 1717 at the bequest of King George I who needed some musical accompaniment for a party he was throwing on the River Thames. Handel knocked out a slew of movements for the occasion, which were later arranged into three giant suites. Thursday evening's performance combined movements from the first and second. A couple of winds and brass added to the overall orchestral size and color.
Handel's Overture is structured like Bach's: a stately beginning and closing surround an animated middle section. The next seven movements vary in tempo and character, and one can get lost as to exactly where one is in the piece, because some movements have repeats and contrasting middle sections. But it doesn't really matter, since this music was designed to be agreeable background music for the king's party.
Frequently the oboe is singled out for some distinct work; other times the French horns (often conjuring up a hunt) and trumpets add some royal flair. The ensemble was good throughout, and some terrific dynamic contrasts were evident.
Vivaldi's The Four Seasons is a collection of four violin concertos. The works are touted as some of the first pieces of "program music," that is music that is inspired by extra-musical elements — in this case, poetry. Each of the four seasons "sets" the events and moods evoked in the accompanying sonnet. (In his opening comments, Sitkovetsky said the music was "like a soundtrack" to the poems.) A special treat was that the poems were read by (Chesley Kennedy) before each concerto was performed.
Sitkovetsky was center-stage, serving as both conductor and soloist. Sometimes only the GSO first chair string players (John Fadial, Fabrice Dharamraj, Scott Rawls, Beth Vanderborgh, and John P. Spuller) accompanied Sitkovetsky, giving the music a lean and intimate feel.
Sitkovetsky's playing contained more theater than sometimes is present. But this music practically demands musical theater: shivering, icy string lines, gruff peasant fiddling. And the Maestro added ornaments not often heard in the piece. Great playing.

redpajama_set_name: RedPajamaCommonCrawl


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Unauthorised resellers may choose to cut corners by repairing instead of replacing critical spare parts.
Untrained technicians may not be able to accurately diagnose problems. They are unable to obtain any latest firmware upgrades and this will deny you improved features.


text:
Saudi Arabia Updates Plans to Mine Its Uranium Deposits
Dan Yurman 126,639
Editor & Publisher, NeutronBytes, a blog about nuclear energy
Publisher of NeutronBytes, a blog about nuclear energy online since 2007. Consultant and project manager for technology innovation processes and new product / program development for commercial...
Jan 13, 2022Jan 13, 2022 11:52 pm GMT
Following on a NYT August 2020 report that the Kingdom of Saudi Arabia (KSA) plans to use technical expertise from Chinese state-owned enterprises to process uranium ore from hard rock mines to make yellowcake, this week (01/13/22) Prince Abdulaziz bin Salman al-Saud told a mining conference in Saudi Arabia that the kingdom plans to use its uranium resources to develop a nuclear power program.
According to a Reuters wire service report, Prince Abdulaziz said that Saudi Arabia would be mining and developing its uranium resources. The actual extent of the commercially viable ore remains uncertain but the intent to pursue the mining venture appears to be quite certain.
"We do have a huge amount of uranium resource, which we would like to exploit and we will be doing it in the most transparent way," Prince Abdulaziz told the Future Minerals Summit in Riyadh.
For the time being the program's public profile is that in terms of the nuclear fuel cycle, it only goes to the extent of turning natural uranium (U308) into yellowcake. So far there has not been an announcement from KSA officials that the country plans to build conversion and enrichment facilities to produce nuclear fuel at commercial levels (U235 at 3-5%) or beyond that point.
The cost of these nuclear fuel facilities is not trivial. They would include hard rock mining operations which would require multiple mines, a mill and a related facility to convert the extracted uranium, perhaps at a rate of 4 pounds per ton of ore, into yellowcake.
Commercially recoverable rates of uranium from ore run from dismal, at less than 1 pound per ton to exceptional, at 11-15 pounds per ton of ore which are found in Saskatchewan, Canada. Knowing how much uranium is available and how much can be retrieved per ton of ore are crucial commercial metrics for making a decision to open a mine and build processing facilities.
It has not been a secret for a long time that Saudi Arabia has deposits of uranium that could be commercially viable to form the basis for mining operations. However, the deposits are not listed in directories of uranium deposits with verified estimates of recoverable quantities.
S&P Global/Platts reported on 1/12/22 that while there are no official figures published on Saudi uranium reserves, in 2020, a report by UK-based newspaper the Guardian, based on leaked internal documents, put the kingdom's "inferred deposits" at an estimated 90,000 mt, which would be equivalent to around 1.4% of current global reserves if verified by subsequent efforts. The prospecting that reports the inferred deposits was carried out by geologists from Chinese state owned enterprises. Their report identified three major sites where potentially uranium could be mined.
The Guardian newspaper reported that Prof Kip Jeffrey, head of Camborne school of mines at the University of Exeter, commented, "If some of these became actually viable deposits – and there's no way of knowing whether that's possible or not – the actual amounts are probably going to be well in excess of what a power plant, or a few power plants would need."
Mark Hibbs, senior fellow in the nuclear policy program at the Carnegie Endowment for Peace, told the newspaper, "If you are considering nuclear weapons development, the more indigenous your nuclear program is, the better. In some cases, foreign suppliers of uranium will require peaceful-use commitments from end users, so if your uranium is indigenous, you don't have to be concerned about that constraint."
Note that in the world of uranium prospecting the U.S. Geological Survey defines "inferred deposits" as the least accurate method of estimating commercially recoverable quantities of uranium from ore. This is the method Saudi Arabia is using to report its recoverable levels of uranium based on prospecting surveys. It means that Saudi Arabia doesn't really know at this stage how much uranium can be taken from their domestic deposits or what the yield will be from the ore.
"Inferred reserves" are those for which quantitative estimates are based largely on broad knowledge of the geologic character of the deposits, and for which there are few, if any, samples or measurements.
By comparison, "indicated reserves" are much more accurate. They are defined as those for which the grade is computed from drill-hole samples, exposures in mine workings and natural outcrops, gamma-ray logs, and production data, and for which the tonnage is computed by projection for a reasonable distance on geologic evidence from points of exposure (drill holes, mine workings, and natural outcrops).
To get to the next step in the nuclear fuel cycle in terms of producing usable nuclear fuel, once you have the ore out of the ground and into a mill, the yellowcake it produces would have to then be sent to a conversion facility to make a gaseous form of uranium hexafluoride (UF6). From there the gaseous form would go to an enrichment facility to extract the fissile U235 isotope to make nuclear fuel (5% U235) Note that bomb material has an enrichment level greater than 80% U235.
The enrichment facility spins the gas in centrifuges at a very high rate of speed to separate the lighter U235 isotope (the fissile material) from the heavier U238 raw uranium. The reason it is called "enrichment" is that U235 in raw uranium is only 0.7% of the mass. It takes a of spinning centrifuges to get to 5% U235 which is the high end for commercial nuclear fuel.
Image: IAEA
Saudi Arabia has none of these facilities and the cost of building them would be several hundred million dollars and take two-to-three years. Yet, Prince Abdulaziz said in his remarks that KSA would consider exporting the yellowcake to other countries which could include its long time partner Pakistan or China.
Saudi Arabia currently has no nuclear power generation plants but has said it will add around 17 GW of nuclear capacity by 2040 and has ambitions to bring two reactors with a combined capacity of 2.8 to 3.2 GWe online within the next decade. Plans to release a tender to bidders for the first two units have repeatedly been pushed back repeatedly although a request for information from potential vendors was distributed several years ago.
Last August there was an indication that the process was underway once again. A Saudi note published in a construction trade press journal requested management consulting support services for the nuclear program indicating the country's energy ministry may be restarting the bid and proposal process.
After a long period of relative quiet, KSA announced in August 2021 that The King Abdullah City for Atomic and Renewable Energy (KACARE) plans to hire the services of a global management service company to advise on Saudi Arabia's first nuclear project in the next two months. The report was monitored on a CNBC Arabia TV channel.
According to the report, the global bidders for the project include Deloitte, Ernst & Young, HSBC and PricewaterhouseCoopers.
KSA does not have a 123 Agreement with the US and has repeatedly affirmed its "right" to develop uranium enrichment and spend fuel reprocessing facilities albeit without have the capacity or budget to build them. In rejecting U.S. nuclear technologies by refusing to sign on to a 123 agreement, KSA has turned to China as a potential partner for new nuclear reactors.
Plans for Making Hydrogen
S&P Global / Platts also reported that KSA has expressed interest in becoming a leader in blue and green hydrogen as it looks at alternative energy sources. Saudi Arabia will adopt a partnership approach towards developing hydrogen, Prince Abdulaziz told the summit.
"We are working with our friends from the EU but we hope that we can aggregate for example, our EU partners to work with us on delivering hydrogen, either it is ammonia [that is] shipped or even piping it," he said.
Saudi Aramco signed agreements last year to develop hydrogen manufactured from electrolysis powered by solar and wind. In 2020, the company shipped a cargo of blue ammonia to Japan, one of its biggest buyers of crude. Ammonia is the currently easiest way to store and transport hydrogen.
nuclear-generation
Dan Yurman
Thank Dan for the Post!
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text:
\section{Introduction}
The mass and non-gravitational interactions of particle dark matter remain unknown. Although many candidates have been proposed, particles that achieve the observed relic abundance through thermal freeze out have garnered the most attention~\cite{Zeldovich1,Zeldovich2,Chiu1}.
While thermal relics are often assumed to have weak-scale masses this does not have to be the case; the thermal freeze-out mechanism works for a much broader range of masses and leaves room for models from keV to multi-TeV masses encompassing the whole experimentally allowed range of cold dark matter.

For thermal relics, an upper bound of approximately $340$~TeV can be set on the dark matter mass using partial wave-unitarity~\cite{Griest:1989wd}. Finding a robust lower bound is more difficult. General theoretical attempts have been made, for example by Hut and Lee-Weinberg~\cite{Hut:1977zn,Lee:1977ua}. However, these can be avoided by keeping the dark matter particle in thermal equilibrium with, for instance, a light mediator~\cite{Boehm:2003hm}, and a robust lower bound requires using experimental constraints. For example, a model independent lower bound for fermionic dark matter of $m\gtrsim1$~keV can be set by considering the phase-space distribution of dark matter in dwarf spheroidal galaxies~\cite{Boyarsky:2008ju}. Structure formation indicates that dark matter cannot be hot so a similar bound of $\mathcal{O}(\rm{keV})$ can be placed by requiring that the free-streaming length is small~\cite{Bond:1983hb}.
A more model dependent lower bound, $m\gtrsim10$~GeV, can be placed by considering distortions due to energy injection by \mbox{$s$-wave} annihilation in the cosmic microwave background (CMB)~\cite{Padmanabhan:2005es,Mapelli:2006ej,Zhang:2006fr,Galli:2009zc,Slatyer:2009yq,Hutsi:2011vx,Galli:2011rz,Finkbeiner:2011dx,Slatyer:2012yq,Lopez-Honorez:2013cua}. However this can be evaded if the annihilation is a $p$-wave process or if the dark matter annihilates to neutrinos. Bounds can also be placed from Big-Bang Nucleosynthesis~\cite{Kolb:1986nf,Serpico:2004nm}, but these suffer from systematic uncertainties in the measured values of the primordial nuclear abundances~\cite{Beringer:1900zz,2012arXiv1208.0032S}.

Here we find a new lower bound for cold thermal dark matter using data from the Planck satellite. The only light states in the Standard Model (SM) that it is possible to  be in thermal equilibrium with are the neutrinos or electrons and photons, and so it is natural to assume that the dark matter will be coupled to these states. If this is the case and the dark matter decouples while non-relativistic, there will be a change in the effective number of neutrinos ($\Neff$) through its effect on the neutrino-photon temperature ratio~\cite{Boehm:2012gr,Ho:2012ug,2013arXiv1303.0049S}.
Using the results from Planck~\cite{Ade:2013lta}, which has measured the CMB angular power spectrum with an unprecedented accuracy, we show that a bound of about an MeV can be placed on the dark matter mass, if the dark matter is in thermal equilibrium with the neutrinos or the electrons and photons after neutrino decoupling. The exact bound depends on whether the dark matter is a scalar or fermion and to which SM species it couples. The advantage of our method is that it works even for a $p$-wave annihilation cross-section and for annihilation to neutrinos - cases when limits such as energy injection into the CMB do not apply.  Previous studies have used $\Neff$ to constrain the mass of dark matter annihilating exclusively into electrons~\cite{Ho:2012ug}. However, that analysis did not take into account the degeneracy of $\Neff$ with helium, which leads to a slightly weaker bound, while ours does. Our analysis using the Planck data supersedes that study and we also consider the case of annihilation into neutrinos.

Our bounds apply to models such as electric dipole and anapole dark matter~\cite{Bagnasco:1993st, Pospelov:2000bq,Sigurdson:2004zp,Masso:2009mu, An:2010kc, Fitzpatrick:2010br,2012arXiv1211.0503H} or to models in~\cite{Boehm:2003bt,Ahn:2005ck,Hooper:2008im} where the dark matter annihilates into electrons or photons, and could be relevant to models which give a signal at electron recoil direct detection experiments~\cite{Essig:2011nj,Essig:2012yx,Graham:2012su}. Fewer models have been constructed where dark matter annihilates into neutrinos. Therefore, as an application of our bounds, we constrain a supersymmetric dark matter model where the dark matter is a light bino-like neutralino and a mixed left-right handed sneutrino plays the role of the light mediator. Annihilation in this model is $p$-wave and the neutralino remains in equilibrium with the neutrinos. We show that a new lower bound can be placed on the neutralino mass of~$3.5$~MeV.

This paper is organised as follows. In section~\ref{sec:lowerneff} we show how light, cold, thermal dark matter annihilating into neutrinos or electrons and photons changes $\Neff$ and derive a bound on the mass of dark matter particle using data from Planck. We compare these bounds with those derived from Big Bang Nucleosynthesis (BBN) and show that they are stronger. Following that, in section~\ref{sec:lightchi} we construct a supersymmetric model where the dark matter is a light bino-like neutralino and a light mixed left-right sneutrino mediates efficient neutralino annihilation into neutrinos.  Appendices discuss changes in the mass bounds when the HST prior on $H_0$ is applied and the collected constraints on our neutralino model from invisible widths of the $Z$- and Higgs boson, rare meson decays, collider direct production and beam dump searches as well as constraints from SN1987A, large scale structure and direct detection experiments.

\section{A lower mass bound from Planck}
\label{sec:lowerneff}
In this section we show how a lower bound can be placed on the mass of cold thermal dark matter by using Planck's constraint on $\Neff$. This bound applies if the dark matter remains in thermal equilibrium with either photons and electrons or neutrinos until after the time when neutrinos decouple from electrons.\footnote{Our bounds do not apply to dark matter candidates that were not in thermal equilibrium with neutrinos, electrons or photons in the early universe. This includes, for instance, primordial black holes~\cite{Ricotti:2007au,Frampton:2010sw,Hawkins:2011qz} and the QCD axion, whose abundance arises from the non-thermal misalignment mechanism~\cite{Preskill:1982cy,Abbott:1982af,Dine:1982ah}. However, non-QCD (heavier) axions can be in thermal equilibrium and can change $\Neff$ (see e.g.~\cite{Cadamuro:2010cz}).}

The effective number of neutrinos, $\Neff$, is a convenient way to parameterise the energy density apart from the photon contribution. It allows us to write the total energy density as
\begin{equation}\label{eq:rhotot}
\rho\equiv\rho_{\gamma}\left[1+\frac{7}{8} \left(\frac{4}{11}\right)^{4/3} \Neff \right]\;.
\end{equation}
The factor $(4/11)^{4/3}$ is the fourth power of the neutrino-photon temperature ratio $T^0_{\nu}/T_{\gamma}=(4/11)^{1/3}$, which assumes instantaneous decoupling of three neutrino species. In the standard cosmological model \mbox{$\Neff=3.046$}, reflecting that the actual neutrino-photon temperature relation is slightly higher due to decoupling effects~\cite{Mangano:2001iu, Mangano:2005cc}.

The standard lore is that a value of $\Neff>3.046$ implies that there must be a new light species that is relativistic when the cosmic microwave photons decouple (at $T\sim1$~eV).\footnote{See refs.~\cite{Brust:2013ova,DiBari:2013dna} for constraints on this class of models using Planck data.} However, this is not the case and thermal dark matter with mass up to $\sim10$~MeV can also change $\Neff$, as we now argue using the example of electrons. In the standard cosmological model, the electrons do not directly contribute to the energy density at recombination because they are non-relativistic at this time. However they do have an effect on $\Neff$ because the electrons caused the photons to develop a higher temperature than the neutrinos. The definition of $\Neff$ assumes that a definite temperature ratio holds, namely that \mbox{$T^0_{\nu}/T_{\gamma}=(4/11)^{1/3}$}. Had the electrons not been present, the photons and neutrinos would have had the same temperature and $\Neff$ would have been larger than three by a factor $(11/4)^{4/3}$.

In a similar fashion, thermal dark matter in thermal equilibrium with photons, electrons or neutrinos can change $\Neff$ by altering the neutrino-photon temperature ratio. In order for this to happen, the dark matter must transfer its entropy to either the electrons and photons or to the neutrinos, after the neutrinos decouple from the electrons at $T_{\rm{D}}\approx2.3$~MeV~\cite{Enqvist:1991gx} (we assume that new interactions do not change the neutrino decoupling temperature). If the dark matter is in thermal equilibrium with photons, electrons and neutrinos after neutrino decoupling, it will reheat them equally and $\Neff$ will not change. Since the entropy transfer occurs when the particle becomes non-relativistic, a change in $\Neff$ occurs if the mass $m\lesssim\text{few}\times T_{\rm{D}}\sim10$~MeV. Cold thermal dark matter automatically satisfies the condition of being in thermal equilibrium until the temperature drops below its mass; typically, MeV-mass thermal dark matter drops out of chemical equilibrium when $T\sim m/15$.\footnote{Our bounds also apply to a sub-component of cold dark matter that is a thermal relic; a thermal sub-component (with MeV-mass) remains in chemical equilibrium until $T\lesssim m/15$.}

\begin{figure*}[t!]
\includegraphics[width=2.05\columnwidth]{Neffplot3.pdf}
\caption{Left panel: $\Neff$ as a function of the cold thermal dark matter mass $m$. The green (red) lines are for the case when the dark matter is in thermal equilibrium with neutrinos (electrons and photons) and show that $\Neff$ increases (decreases) as $m$ is reduced. Right panel: The blue regions show the $68\%$ and $95\%$ regions determined from Planck+WP+highL+BAO when both $\Neff$ and $Y_p$ are varied freely. The green (red) lines indicate the relationship between $Y_p$ and $\Neff$ for particles in thermal equilibrium with neutrinos (electrons and photons). As $m$ decreases, the prediction for $\Neff$ and $Y_p$ falls outside of the Planck confidence regions.}
\label{fig:mNeff}
\end{figure*}

We now put the above argument on a more quantitative footing. We first consider the case where the dark matter is in thermal equilibrium with neutrinos. The case where it is in equilibrium with electrons and photons then follows in a straightforward fashion. The contribution of $N_{\nu}$ neutrinos and $n$ particles (with mass $m_i$ and internal degrees of freedom $g_i$) in thermal equilibrium with the neutrinos to the energy density is
\begin{equation}\label{eq:rhonu}
\frac{\rho_{\nu+n}}{\rho_{\gamma}}=\frac{7}{8}\left(\frac{T_{\nu}}{T_{\gamma}}\right)^4 \left[N_{\nu}+\sum_{i=1}^n\frac{g_i}{2} I \left( \frac{m_i}{T_{\nu}}\right) \right]\;,
\end{equation}
where
\begin{align}
\label{eq:Iy}
I(x)=\frac{120}{7 \pi^4} \int^{\infty}_x dy \frac{y^2 \sqrt{y^2-x^2}}{e^{y}\pm1}
\end{align}
with limits $I(\infty)=0$ and $I(0)=1(8/7)$ for fermions (bosons) respectively. As usual, the sign $+\,(-)$ refers to fermion (boson) statistics. In general, $T_{\nu}\neq T_{\nu}^0$. We allow for $n$ particles as, in addition to the cold thermal dark matter, there may be light mediators that also contribute to the energy density. Comparing eqs.~\eqref{eq:rhotot} and~\eqref{eq:rhonu}, we see that
\begin{equation}
N_{\rm{eff}}=\left(\frac{4}{11}\right)^{-4/3}\left(\frac{T_{\nu}}{T_{\gamma}}\right)^{4} \left[N_{\nu}+\sum_{i=1}^n\frac{g_i}{2} I \left( \frac{m_i}{T_{\nu}}\right)   \right]\;.
\label{eq:Neff1}
\end{equation}
Anticipating that the bound on $m_i$ is such that $m_i\gg T_{\nu}(\text{at recombination})\sim1$~eV, we set $I(m_i/T_{\nu})=0$ so that
\begin{equation}
N_{\rm{eff}}=N_{\nu} \left(\frac{4}{11}\right)^{-4/3}\left(\frac{T_{\nu}}{T_{\gamma}}\right)^{4}\;.
\label{eq:Neff2}
\end{equation}

The ratio $T_{\nu}/T_{\gamma}$ is determined by considering entropy conservation (see e.g.~\cite{Kolb:1986nf,Srednicki:1988ce,Boehm:2012gr}). After neutrino decoupling at $T_{\rm{D}}\approx 2.3$~MeV, the entropy of the `neutrino plasma' and `electromagnetic plasma' are separately conserved so that (for $T_{\gamma}<T_{\rm{D}}$)
\begin{equation}\label{eq:Tnugamma}
\frac{T_{\nu}}{T_{\gamma}}=\left(\left. \frac{g_{\star s: \nu}}{g_{\star s: \gamma}}\right|_{T_{\rm{D}}} \frac{g_{\star s: \gamma}}{g_{\star s: \nu}} \right)^{1/3}\;.
\end{equation}
Here $\left.\right|_{T_{\rm{D}}}$ indicates that $g_{\star s}$ should be evaluated at the neutrino decoupling temperature $T_{\rm{D}}$ while $g_{\star s: \nu}$ and $g_{\star s: \gamma}$, defined through $s_{\nu}=2 \pi^2 g_{\star s: \nu} T_{\nu}^3/45$ and $s_{\gamma}=2 \pi^2 g_{\star s: \gamma} T_{\gamma}^3/45$ respectively, are the effective number of relativistic degrees of freedom in the neutrino and electromagnetic plasmas. Explicitly,
\begin{equation}
g_{\star s:\nu}= \frac{14}{8}\left[ N_{\nu}+\sum_{i=1}^n \frac{g_{i}}{2} F\left(\frac{m_i}{T_{\nu}}\right)\right]\;.
\label{gstarsnu}
\end{equation}
where
\begin{equation}
F(x)=\frac{30}{7 \pi^4}\int^{\infty}_x dy \frac{(4 y^2-x^2)\sqrt{y^2-x^2}}{e^{y}\pm1}\;.
\end{equation}
with limits $F(\infty)=0$ and $F(0)=1(8/7)$ for fermions (bosons) respectively and the sign $+\,(-)$ refers to fermion (boson) statistics.

Again, anticipating that the bound on $m_i$ is such that $m_i\gg T_{\nu}(\text{at recombination})\sim1$~eV, we find that for particles only in thermal equilibrium with neutrinos, eq.~\eqref{eq:Neff2} simplifies to
\begin{equation}
\label{eq:Neff3}
N_{\rm{eff}}^{\mathrm{Equil.}\, \nu}=N_{\nu} \left[1+\frac{1}{N_{\nu}}\sum_{i=1}^n \frac{g_{i}}{2} F\left(\frac{m_i}{T_{\rm{D}}}\right)\right]^{4/3}
\end{equation}

For the case of particles in thermal equilibrium with electrons or photons, we again find eq.~\eqref{eq:Neff2} and can use eq.~\eqref{eq:Tnugamma} to find the new temperature ratio. In this case, we find
\begin{equation}
\label{eq:Neff4}
N_{\rm{eff}}^{\rm{Equil.}\, \gamma/e}=N_{\nu} \left[ 1+\frac{7}{22}\sum_{i=1}^n \frac{g_i}{2} F\left( \frac{m_i}{T_{\rm{D}}}\right) \right]^{-4/3}
\end{equation}
where we have used $F\left(m_e/T_{\rm{D}}\right)\approx1$.

The dot-dashed, dashed, dotted and solid lines in the left panel of fig.~\ref{fig:mNeff} show the value of $\Neff$ for a single particle of mass $m$ for a Dirac fermion, Majorana fermion, complex scalar and real scalar respectively. The case where the particle is in equilibrium with neutrinos is shown by the green lines. Here, $\Neff$ increases above the standard value of $\Neff=3.046$ for particles lighter than~$\simeq 20$ MeV. Conversely, $\Neff$ decreases below the standard value for particles in equilibrium with electrons and photons, as indicated by the red lines. There is no effect above $m\geq20$~MeV because the entropy transfer occurs before the electromagnetic and neutrino plasmas decouple resulting in the standard neutrino-photon temperature ratio.

With eqs.~\eqref{eq:Neff3} and~\eqref{eq:Neff4} we can put a bound on the dark matter mass by requiring that $\Neff$ is compatible with the measured value from Planck. The central result from~\cite{Ade:2013lta},
\begin{equation}\label{eq:Neffplanck}
\Neff=3.30^{+0.54}_{-0.51}\quad(\text{95\%; Planck+WP+highL+BAO}),
\end{equation}
which combines Planck precision measurement of the CMB, WMAP-9's polarisation data (WP)~\cite{Bennett:2012fp}, SPT's high-$\ell$ measurement (highL)~\cite{Reichardt:2011yv} and baryon acoustic oscillations (BAO) measurements from large scale structure surveys~\cite{Percival:2009xn,Padmanabhan:2012hf,Blake:2011en,Anderson:2012sa,Beutler:2011hx} cannot be used to set an accurate constraint on this scenario. This is because this result assumes that all of the relativistic components parameterised by $\Neff$ consist of free streaming relativistic particles which are effectively massless. In particular, the helium abundance $Y_p$ is fixed to the BBN theory prediction for effectively massless relativistic particles. As was first described in \cite{Kolb:1986nf}, this relation does not hold in our case: the new particles alter the standard prediction for $Y_p$ from relativistic particles because the additional semi-relativistic particles and the change in the neutrino-photon temperature ratio both contribute to the energy density during BBN. The difference in this relationship is important because the impact of $Y_p$ on the damping tail of the power spectrum is degenerate with the effect from $\Neff$ (see e.g.~\cite{Hou:2011ec} for further discussion).

Therefore, we use the results from the Planck+WP+highL+BAO analysis in which $Y_p$ and $\Neff$ are simultaneously constrained. The $68\%$ and $95\%$ confidence regions from this analysis are shown in the right panel of fig.~\ref{fig:mNeff}. The green and red lines overlying these regions are our calculations for $Y_p$ (to be discussed in detail in the next section) against $\Neff$ for the cases of particles in equilibrium with neutrinos and electrons or photons respectively. As the mass $m$ of these particles decreases, the prediction for $\Neff$ eventually falls outside the Planck $95\%$ confidence region. Particles lighter than this are excluded at the $95\%$ confidence level.

Requiring that $\Neff$ is consistent with the Planck result, we exclude the following particle masses at $95\%$~C.L.\ for cold thermal dark matter particles in equilibrium with neutrinos:
\begin{align}
&\text{Real scalar}\;&\text{No constraint} \label{eq:nu_RScalarBound}\\
&\text{Complex scalar}\;&m<3.9~\text{MeV}\\ \label{eq:MajFermBound}
&\text{Majorana fermion}\;&m<3.5~\text{MeV}\\
&\text{Dirac fermion}\;&m<7.3~\text{MeV}\label{eq:nu_DirFermBound}
\end{align}
Similarly, we can exclude the following cold thermal dark matter particle masses at $95\%$~C.L.\ when in equilibrium with electrons and photons:
\begin{align}
&\text{Real scalar}\;&0.4~\text{MeV}<m<2.6~\text{MeV}\label{eq:e_RScalarBound}\\
&\text{Complex scalar}\;&m<6.5~\text{MeV}\\
&\text{Majorana fermion}\;&m<6.4~\text{MeV}\\
&\text{Dirac fermion}\;&m<9.4~\text{MeV}\label{eq:e_DirFermBound}
\end{align}

Had we set the limits with eq.~\eqref{eq:Neffplanck}, the bounds would be about $30\%$ higher. These bounds are independent of whether the annihilation cross-section is $s$- or $p$-wave, but there are ways to evade them. We mention three: firstly, the dark matter's abundance might arise from a non-thermal mechanism so that agreement with the Planck limit is found. Secondly, while dark matter in thermal equilibrium with electrons and photons would by itself decrease $\Neff$, the presence of some extra relativistic degrees of freedom (`dark radiation' or sterile neutrinos) would increase $\Neff$ bringing it back into agreement with the Planck result~\cite{2012arXiv1212.1689H,2013arXiv1303.0049S,Drewes:2013gca}. Thirdly, the dark matter could be in thermal equilibrium with electrons, neutrinos and photons in which case there is no change in the standard neutrino-photon temperature ratio and hence, no change in $\Neff$. However, the BBN bounds on the second scenario will be more stringent since the dark matter and the extra degrees of freedom both increase $Y_p$ and there are strong constraints from $\nu-e$ scattering (see e.g.~\cite{Auerbach:2001wg, Formaggio:2013kya}) on the third scenario.

Finally, although we considered here the degeneracy of $Y_p$ and $\Neff$, it is also the case that $\Neff$ is positively correlated with the Hubble constant $H_0$. The Planck measurement of $H_0$ is about $2.5 \sigma$ lower than direct astrophysical measurements. When the astrophysical measurements of $H_0$ are used as a prior, slightly higher values of $\Neff$ are preferred. For completeness, we give the resulting mass bounds in appendix~\ref{app:H0}.

\subsection{Comparison with Big Bang Nucleosynthesis}
\label{app:BBN}
\begin{figure*}[t!]
\includegraphics[width=2.05\columnwidth]{BBN4.pdf}
\caption{ The left [right] panels show the calculated abundances of helium (upper segment) and deuterium (lower segment) for cold dark matter in thermal equilibrium with neutrinos [photons and electrons] respectively. The dotted lines label by $N_{\nu}$ show the predicted abundances for $N_{\nu}$ massless neutrinos.}
\label{fig:BBN}
\end{figure*}

A bound on the dark matter mass can also be placed by comparing the primordial abundance of helium and deuterium predicted from BBN with the observed values. Here we compare those bounds with those we have just derived from Planck's measurement of $\Neff$. Unfortunately, the observed values of primordial helium and deuterium are beset by large systematic errors and various central values and errors appear in the literature. Following the convention in the rest of particle physics, we take the values recommended in the PDG review of BBN~\cite{Beringer:1900zz}:
\begin{align}
\label{PDG:BBN}
Y_p&=0.249 \pm 0.009\\
\rm{D}/\rm{H}&=(2.81 \pm 0.21) \times 10^{-5}\;.
\end{align}

We calculate $Y_p$ and $\rm{D}/\rm{H}$ as a function of particle mass $m$ with a modified version of the $\texttt{PArthENoPE}$ BBN code~\cite{Pisanti:2007hk}. As well as including the energy density of the additional particle, the effects of the change in the neutrino-photon temperature relation must also be accounted for. This includes, for instance, a modification of the interaction rates for $p \leftrightarrow n$ which change the ratio of the neutron-to-proton number density. We refer the reader to~\cite{Serpico:2004nm,Boehm:2012gr} for a detailed description of how these effects are implemented.

\begin{table}[t!]
\centering
\begin{tabular}{l c c c}
\hline
\multicolumn{4}{c}{Equilibrium with $\nu$} \\
	 & Planck & $Y_p$ \;\;&D/H  \\[0.3ex]
\hline \\[-1.0em]
 Real scalar 		& -- & -- \;\;& --  \\
Complex scalar 	& 3.9  & -- \;\;& -- \\
Majorana fermion	& 3.5 & -- \;\; & --  \\
Dirac fermion		& 7.3 & 0.8 \;\;& 3.3 \\[0.5ex]
\hline
\multicolumn{4}{c}{Equilibrium with $\gamma / e$} \\
	 & Planck & $Y_p$ \;\;&D/H  \\[0.5ex]
\hline  \\[-1.0em]

 Real scalar 		& $0.4 \leq m \leq 2.6$ & -- \;\;& 0.4 \\
Complex scalar 	& 6.5  & 0.2 \;\;& 0.5 \\
Majorana fermion	& 6.4  & 0.2 \;\;& 0.5 \\
Dirac fermion		& 9.4  &0.3 \;\; & 5.3 \\[0.5ex]
\hline
\end{tabular}
\caption{The upper (lower) table show the 95\% C.L.~bounds on the dark matter mass $m$ for particles in equilibrium with neutrinos (electrons and photons). The numbers are an upper bound unless stated otherwise, `--' indicates that there is no limit  and the units are MeV. Generally, the limit from D/H is stronger than the limit from $Y_p$, while Planck is stronger than both.}
\label{tab:bounds}
\end{table}

The abundances for $Y_p$ and D/H are shown in the upper and lower segments of fig.~\ref{fig:BBN} respectively. In calculating these values, we have taken $\Omega_b h^2=0.0224$ and $\tau_n=880.1$~s, as recommended by the PDG~\cite{Beringer:1900zz}. The left and right panels show the results for particles in thermal equilibrium with neutrinos and electrons or photons respectively. The dotted lines labelled by $N_{\nu}$ show the predicted abundances for $N_{\nu}$ massless neutrinos.

The resulting masses that can be excluded at the $95\%$~C.L.\ are given in table~\ref{tab:bounds}. Numbers quoted are in units of MeV. The bounds from D/H are generally stronger than those from $Y_p$ but both are weaker than the Planck bounds. The only exception is for a real scalar in thermal equilibrium with photons and electrons. With the combination of the D/H and Planck bounds, the region $m<2.6$~MeV is excluded.

\section{Application: light neutralino dark matter}
\label{sec:lightchi}
We now consider the application of the above bounds to a specific cold thermal dark matter candidate. In our model, the dark matter candidate is a light bino-like neutralino which remains in thermal equilibrium with neutrinos through stronger than weak interactions
mediated by a light mixed left-right handed sneutrino. The annihilation cross-section is $p$-wave suppressed and the above bound provides the strongest constraint on the mass.

The natural expectation for the mass of the lightest neutralino is about the weak scale, $\mathcal{O}(100)$~GeV. However the absence of any signal of supersymmetry (SUSY) at the Large Hadron Collider (LHC) may indicate that the much-studied usual mechanisms of SUSY breaking are not realised, and/or that some tuning may be required. Yet SUSY with $R$-parity still has many desirable features, such as gauge coupling unification, and may still tame most of the electroweak hierarchy problem. It also provides a flexible framework that is extremely useful to explore possibilities for the dark matter parameter space. In light of these arguments, we consider an extension of the MSSM with a spectrum which is dramatically different from those considered in standard SUSY model building (summarised in fig.~\ref{fig:spectrum}).

In the MSSM, the lightest neutralino is a superposition of bino ($\tilde{B}$), neutral wino ($\tilde{W}^0$) and neutral higgsinos ($\tilde{h}_d^0$ and $\tilde{h}_u^0$):
\begin{equation}
\nuchi=N_{11} \tilde{B}+N_{12} \tilde{W}^0+N_{13} \tilde{h}_d^0+N_{14} \tilde{h}_u^0\;,
\end{equation}
where $N_{1i}$ are the components of the neutralino mixing matrix~\cite{Dreiner:2008tw}. Searches at LEP impose a lower bound on $M_2$, which, when the GUT relation $M_1=5 \tan^2\theta_W M_2/3\approx M_2/2$ is imposed, translate into a lower bound on $M_1$; in this case a lower bound of 46~GeV can be placed on the mass of the lightest neutralino~\cite{Abdallah:2003xe,Beringer:1900zz}. However, when this assumption is relaxed and $M_1$ and $M_2$ are treated as independent parameters, a massless neutralino is not ruled out by laboratory, astrophysical or cosmological limits if it is bino-like~\cite{Bartl:1989ms, Choudhury:1999tn,Kachelriess:2000dz, Gogoladze:2002xp,Dreiner:2003wh, Dreiner:2009ic,Dreiner:2009er}. Therefore, here we consider the case when the dark matter is, for all purposes, purely bino-like.

In this paper we remain agnostic as to the exact mechanism that gives rise to a light neutralino. However, we briefly mention two mechanisms by which this could arise. First, a light bino-like neutralino can be obtained if there is a hierarchy between $M_1$ and $(M_2, \mu)$. This arises, for instance, in hybrid models of SUSY breaking~\cite{Dudas:2008eq}. In this case, in the limit $M_2, \mu \gg m_Z, M_1$, at tree-level the lightest neutralino mass is given by
\begin{equation}
m_{\nuchi}\approx N_{11}^2 \left|M_1 - \sin(2\beta)\sin^2 \theta_W \frac{m_Z^2}{\mu}\right|
\end{equation}
and the bino-component is
\begin{align}
|N_{11}&|\approx\left[1+\sin^2\theta_W \left( \frac{m_Z}{\mu} \right)^2 \right]^{-1/2}  \\
&\approx 1-0.01\left(\frac{300\text{ GeV}}{\mu} \right)^2\;.
\end{align}
The higgsino components are sub-dominant: \mbox{$|N_{13}|\approx \sin \beta \sqrt{1-N_{11}^2}$} and \mbox{$|N_{14}|\approx \cos \beta \sqrt{1-N_{11}^2}$} respectively, while the wino-component is negligible: \mbox{$N_{12}\approx\mathcal{O}(N_{11} M_1/M_2)$}.

Second, we can invoke a symmetry argument. In SUSY models with an $R$-symmetry, gaugino soft-masses are forbidden (Dirac masses are required for the wino and gluino but the bino does not require them). However, it is expected that supergravity effects violate the (global) $R$-symmetry giving rise to a light bino-like neutralino, such as in~\cite{Davies:2011mp}. In that article the Majorana neutralino mass is
\begin{equation}
M_1=\frac{11 \alpha}{4 \pi \cos^2 \theta_W}\,m_{3/2}\approx 9\times10^{-3}\,m_{3/2}\;.
\end{equation}
and the neutralino is totally bino-like. If the gravitino mass is low, $\mathcal{O}(100)$~GeV or less, then the lightest neutralino will be at the MeV scale.

\subsection{Thermal neutralino dark matter}
\label{sec:thermal}
The arguments of Hut~\cite{Hut:1977zn} and Lee-Weinberg~\cite{Lee:1977ua} suggest that a neutralino lighter than $\mathcal{O}(10)$~GeV cannot have the correct thermal relic abundance in the MSSM as all mediators with Standard Model particles are $\mathcal{O}(100)$~GeV. Indeed, detailed studies have borne this out~\cite{Hooper:2002nq, Bottino:2002ry, Belanger:2003wb}. We will therefore need to consider an extension of the MSSM which has a new light mediator in order to keep the neutralino in equilibrium with the thermal bath for longer.\footnote{Of course, this not the only option for a light neutralino to obtain the observed relic abundance: it could occur via a non-thermal mechanism or some source of entropy could dilute the neutralino overabundance.} The light neutralino can only annihilate to those states present in the early universe, namely electrons, photons and neutrinos. We choose as our mediator a light mixed left-right handed sneutrino, which keeps the neutralino in equilibrium with neutrinos through the diagrams shown in fig.~\ref{fig:Feynmandiagrams}. The mixing with a sterile right-handed component is necessary because the left-handed sneutrino couples strongly with the $Z$-boson. Constraints from the $Z$-width prevent it from being lighter than $m_Z/2$ (this is discussed in greater detail in appendix~\ref{app:particleconstraints}).

\begin{figure}[t]
\includegraphics[width=0.99\columnwidth]{relic1.pdf}
\caption{Feynman diagrams showing the interaction that keep the neutralino in chemical equilibrium with the neutrinos in the early universe. The mediator $\tnu$ is a light mixed left-right handed sneutrino.}
\label{fig:Feynmandiagrams}
\end{figure}

Therefore, in addition to the MSSM matter content we introduce three right-handed neutrino superfields $N_i$, which are gauge singlets with respect to the Standard Model gauge symmetries. In addition to the usual MSSM superpotential terms, we also include\begin{equation}
\Delta \mathcal{W}= Y^{\nu}_{ij}\, H_u \cdot L_i N_j \;,
\end{equation}
where $L_i$  is left-handed leptonic chiral superfield, $H_u$ is the up-type Higgs superfield and for $SU(2)$-doublets, our notation is $A\cdot B= A^2 B^1-A^1 B^2$. When the scalar component of $H_u$ gets a vev $(h_u=v \sin \beta)$, where $v=174$ GeV, this gives rise to a Dirac mass for the neutrinos. Therefore, the magnitude of the entries $Y$ are approximately $Y^{\nu}_{ij} \sim 10^{-12}$, and this matrix is diagonalised by the PMNS matrix~\cite{Pontecorvo:1957qd,Pontecorvo:1967fh,Maki:1962mu}. We do not consider a Majorana mass term in this article.\footnote{A Majorana neutrino mass term could be generated radiatively along the lines of~\cite{ArkaniHamed:2000bq, ArkaniHamed:2000kj,Borzumati:2000mc,Borzumati:2000ya, Arina:2007tm, MarchRussell:2004uf, MarchRussell:2009aq} by including a supersymmetric mass term $m_N NN$ and the accompanying soft $B$-term in the scalar potential. We do not investigate this further.}

With the additional soft terms, the left- and right-handed sneutrino contribution to the scalar potential is
\begin{equation}
V_{\rm{soft}}\supset m^2_{\tilde{\nu}_L} |\tilde{\nu}_{Li}|^2+ m^2_{\nur} |\nur_i|^2 + A_{ij}  h_u \cdot \tilde{L}_i \nur_j +\rm{h.c.}\;.
\end{equation}
For simplicity we have assumed that $m^2_{\tilde{\nu}_L}$ and $m^2_{\tilde{n}}$ are generation independent and that $A_{ij}$ has real entries with the same flavour structure as $Y^{\nu}_{ij}$. Therefore, $A_{ij}$ is also diagonalised by the PMNS matrix. This means that
after diagonalising $A_{ij}$, the sneutrino eigenstates $\tilde{\nu}^{\alpha}_{L}$ and $\tilde{n}^{\alpha}$ have the same flavour structure as the neutrinos. For instance, the neutrino mass eigenstate $\nu_2$ has approximately equal electron, muon and tau flavour so $\tilde{\nu}^2_{L}$ and $\tilde{n}^{2}$ also have approximately equal electron, muon and tau flavour.

The diagonal $A_{\alpha}$ terms induce mixing between the left- and right-handed eigenstates (without changing the flavour structure) so that the lightest mass eigenstate is
\begin{equation}
\tnu=-\sin\theta_1\; \tilde{\nu}^{\alpha}_{L}+\cos\theta_1\; \tilde{n}^{\alpha \star}
\end{equation}
with mass \begin{equation}
m^2_{\tnu}=\frac{m_{\tilde{n}}^2 \cos^2\theta_1-m_{\tilde{\nu}_{L}}^2 \sin^2\theta_1}{\cos 2\theta_1}\;.
\end{equation}
The mixing angle is given by
\begin{equation}\label{eq:mixingangle}
\tan 2\theta_i=\frac{2 A_i v \sin \beta}{m_{\tilde{\nu}_{L}}^2-m_{\tilde{n}}^2}\;.
\end{equation}
 For definiteness, we assume that the flavour index is $\alpha=2$ for the lightest mass eigenstate so that it couples to the electron, muon and tau neutrinos with equal strength (to a good approximation). In the remainder of the paper, we drop the subscript `1' on the mixing angle of the lightest mass eigenstate.

The left-handed sneutrino mass-term, $m_{\tilde{\nu}_{L}}=\tilde{m}_{L}^2+\frac{1}{2}\cos(2\beta) m_Z^2$, shares the soft-mass $\tilde{m}_{L}$ with the left-handed selectron so that the ATLAS bound \mbox{$m_{\tilde{e}_L}\gtrsim195$~GeV}~\cite{Aad:2012pxa} implies that $m_{\tilde{\nu}_{L}}\gtrsim200$~GeV. Therefore, to have a light sneutrino requires the relation $m_{\tilde{n}}\approx\tan\theta m_{\tilde{\nu}_{L}}$.  We assume that this cancellation occurs accidentally for the lightest sneutrino while the others remain at $\mathcal{O}(100)$~GeV. To achieve such a mass requires a tuning comparable to that required in the electroweak sector of the CMSSM~\cite{Buchmueller:2011ab,Buchmueller:2012hv}.

To summarise, the neutralino and sneutrino mass spectrum is shown in fig.~\ref{fig:spectrum}. In addition to the light bino-like neutralino, we also have a light mixed left-right handed sneutrino. We assume that all other sparticles, including the heavier sneutrinos and neutralinos are heavy enough to be consistent with direct search bounds from the LHC and LEP.

 \begin{figure}[t]
\includegraphics[height=0.88\columnwidth]{spectrum2b.pdf}
\caption{A schematic diagram showing the structure of the neutralino and sneutrino sectors that we consider in this paper. As well as a sub-GeV bino-like neutralino, we have a light mixed left-right handed sneutrino. The other neutralinos and mixed sneutrinos have soft masses around the electroweak scale $\mathcal{O}(100)$~GeV. We assume that the other sparticles are heavy enough to have evaded direct search constraints from the LHC and LEP.}
\label{fig:spectrum}
\end{figure}

\begin{figure}[t]
\includegraphics[height=0.88\columnwidth]{mass.pdf}
\caption{The mixed sneutrino mass $m_{\tnu}$ required to achieve $\Omega_{\nue}h^2=0.11$ as a function of the neutralino mass $m_{\nue}$ for three different values of $\sin\theta$. The upper dashed blue line is for $\sin\theta=0.1$, the middle solid red line for $\sin\theta=0.06$, and the bottom dash-dotted black line for $\sin\theta=0.04$. The required sneutrino mass is typically $m_{\tnu}\sim\text{few}\times m_{\nue}$. }
\label{fig:relicabundance}
\end{figure}

We turn now to the calculation of the relic abundance. The dominant interaction contributing to neutralino annihilation with the neutrinos is the $t$- and $u$-channel exchange of the mixed sneutrino shown in fig.~\ref{fig:Feynmandiagrams}. In the non-relativistic limit, $t\approx u \approx-m_{\nue}^2$ and the resulting $p$-wave thermally averaged annihilation cross-section is
\begin{align}
\langle \sigma_{\rm{ann}} v \rangle &=\frac{G_F^2 m_Z^4 \sin^4\theta_W}{\pi}\frac{ |N_{11}|^4 \sin^4\theta}{(m_{\tnu}^2+m_{\nue}^2)^2} \frac{m_{\nuchi}^2}{x}\\
&\approx \frac{103 \text{ pb}}{x} \left(\frac{\sin\theta}{0.1}\right)^4 \left(\frac{m_{\nue}}{5\text{ MeV}}\right)^2 \left(\frac{35 \text{ MeV}}{m_{\tnu}}\right)^4\;,
\label{eq:sigmav}
\end{align}
where as usual, $x=m_{\nue}/T$. Using the well known analytic approximation for $p$-wave annihilation, for instance see~\cite{KolbTurner} for details, we find that the thermal relic abundance is
\begin{equation}
\Omega_{\nue}h^2=0.15 \left(\frac{s_0}{2889.23 \text{ cm}^{-3}} \right)\frac{\sqrt{g_{\star }|_{x_{\rm{f}}}} \left(x_{\rm{f}}/15\right)^{2} }{g_{\star s}|_{x_{\rm{f}}} \left(\tilde{\sigma}_0/100\, \rm{pb}\right)}\;,
\end{equation}
where $\tilde{\sigma}_0$ is defined through $\langle \sigma_{\rm{ann}} v \rangle = \tilde{\sigma}_0 x^{-1}$ and
\begin{equation}
\begin{split}
x_{\rm{f}}&=\ln \left[0.076 g g_{\star}^{-1/2}m_{\rm{pl}}m_{\nue}\tilde{\sigma}_0\right]\\
&\qquad-\frac{3}{2}\ln \left\{\ln\left[0.076 g g_{\star}^{-1/2}m_{\rm{pl}}m_{\nue}\tilde{\sigma}_0\right] \right\}.
\end{split}
\end{equation}
We have explicitly left in the dependence on today's entropy density
\begin{equation}
s_0=2889.23\,{\rm{cm}}^{-3}\left(\frac{g_{\star s}}{3.9091}\right),
\end{equation}
because the light neutralino and light sneutrino lead to a change in the present day value of \mbox{$g_{\star s}=2+21T_{\nu}/(4 T_{\gamma})$}, through the change in the neutrino-photon temperature ratio (see eq.~\eqref{eq:Tnugamma}).

Figure~\ref{fig:relicabundance} shows the sneutrino mass $m_{\tnu}$ required to achieve the relic abundance $\Omega_{\nue}h^2=0.11$ as a function of the neutralino mass $m_{\nue}$ for three different values of $\sin\theta$. For $\sin\theta\gtrsim0.05$, the required sneutrino mass is $m_{\tnu}\sim\text{few}\times m_{\nue}$. For sufficiently small values of $\sin\theta$, the required sneutrino mass is smaller than the neutralino mass so that the neutralino can no longer be the dark matter. For instance, for $\sin\theta=0.04$, the  sneutrino mass (required to achieve the observed relic abundance) is approximately the same as the neutralino mass at $\sim 19$~MeV. In this article we do not consider the case where the mixed sneutrino is lighter than the neutralino (and thus, potentially, the dark matter particle), although we note that similar bounds deriving from $\Neff$ will also apply in that case.

\begin{figure}[t]
\includegraphics[width=0.99\columnwidth]{Neff2.pdf}
\caption{The three lines show $\Neff$ as a function of the neutralino mass $m_{\chi}$ for three choices of $\sin\theta$. The sneutrino mass $m_{\tnu}$ has been set to the value in fig.~\ref{fig:relicabundance} so that $\Omega_{\nue}h^2=0.11$. The green shaded area shows the 95\% confidence region $2.52\leq \Neff \leq 4.14$ from the Planck satellite in combination with WMAP-9's polarisation data, SPT's high-$\ell$ data and BAO measurements. We exclude $m_{\nue}\gtrsim3.5$~MeV. The difference in the behaviour of the lines is due to the sneutrino, which contributes when $m_{\tnu}\lesssim10$~MeV.}
\label{fig:bound}
\end{figure}

\subsection{Constraining the model}
In appendix~\ref{app:particleconstraints} we have collected together constraints on this model from invisible widths of the $Z$- and Higgs boson, rare meson decays, collider direct production and beam dump searches as well as constraints from SN1987A, large scale structure and direct detection experiments. These constraints imply that the neutralino must be bino-like and the sneutrino mixing angle \mbox{$\sin\theta\lesssim0.11$}. However, these do not provide us with any constraint on the mass of the neutralino dark matter, apart from the $\mathcal{O}$(keV) mass bound from free streaming and phase space arguments mentioned in the introduction.

Therefore, we now use the $\Neff$ bound from section~\ref{sec:lowerneff} to show that this provides the strongest mass constraint for neutralino dark matter in this model, improving the previous lower bound by three orders of magnitude. Since both the neutralino and sneutrino remain in thermal equilibrium with the neutrinos after they decouple, we can use eq.~\eqref{eq:Neff3} to show
\begin{equation}
N_{\rm{eff}}=3.046 \left[1+\frac{F\left(m_{\nue}/T_{\rm{D}}\right)+F\left(m_{\tnu}/T_{\rm{D}}\right)}{3.046}\right]^{4/3}.
\end{equation}

In fig.~\ref{fig:bound} we plot $\Neff$ as a function of $m_{\nue}$ for the same values of $\sin \theta$ as in fig.~\ref{fig:relicabundance}. The same colour coding is also used in this figure. The sneutrino mass $m_{\tnu}$ has been fixed to the value shown in fig.~\ref{fig:relicabundance} for a given value of $m_{\nue}$ and $\sin\theta$. The shaded green band in fig.~\ref{fig:bound} shows the $95\%$ allowed range of $\Neff$ taken from fig.~\ref{fig:mNeff}, from the Planck analysis including WMAP-9's polarisation data, SPT's high-$\ell$ data and BAO measurements. We find a lower bound $m_{\nue}\gtrsim3.5$~MeV, consistent with the value quoted in eq.~\eqref{eq:MajFermBound} for the case of Majorana fermion dark matter. When the the sneutrino mass drops below $\sim10$~MeV, it can also contribute to $\Neff$. This explains why the three lines behave slightly differently and why the bound when $\sin\theta=0.04$ is slightly weaker.

In order to use the constraint on $\Neff$, we have implicitly assumed that the neutrinos decouple at \mbox{$T_{\rm{D}}=2.3$~MeV} and the neutralino and sneutrino are only in thermal equilibrium with neutrinos. We now show that this is indeed the case.

The neutralino and sneutrino do not lead to a new interaction between electrons and neutrinos that is stronger than the weak interaction. Therefore, the only change in the decoupling temperature occurs because the expansion rate is slighter faster due to the presence of additional relativistic particles~\cite{2012arXiv1212.1689H}. Neutrinos decouple when $\Gamma\sim G_F^2 T_{\rm{D}}^5=1.66 g_{\star}^{1/2} T_{\rm{D}}^2/m_{\rm{pl}}$. The extra neutralino and sneutrino slightly change $T_{\rm{D}}$ because they contribute to $g_{\star}$. Therefore, the ratio of old and new decoupling temperatures equals the ratio of old and new values of $g_{\star}^{1/6}$. This change is always very small. For instance, taking $m_{\nue}=5$~MeV and $m_{\tnu}=20$~MeV, we find the neutrino decoupling temperature increases to $1.02 \,T_{\rm{D}}$.

We now show that the neutralino and sneutrino are only in thermal equilibrium with neutrinos for temperatures below $T_{\rm{D}}$. In order for this to happen, we have to show that the neutralino and sneutrino are no longer in kinetic equilibrium with the electrons at $T_{\rm{D}}\approx2.3$~MeV. We first consider the neutralino elastically scattering with electrons. The rate of elastic scattering is
\begin{equation}
\Gamma_{\rm{el}}=\langle \sigma_{\nue e} v\rangle n_e\;,
\end{equation}
where $\langle \sigma_{\nue e} v\rangle$ is the thermally averaged elastic scattering cross-section and $n_e$ is the electron number density. The temperature when the last elastic scattering occurs is found from solving $\Gamma_{\rm{el}}=H$, where $H$ is the Hubble expansion rate. However, if the neutralino is non-relativistic, it drops out of kinetic equilibrium before this time because the typical momentum transfer in a single collision, $\Delta p_{\nue}/p_{\nue}\approx \sqrt{3/2}\,T/m_{\nue}$, is small compared to the momentum of the neutralino~\cite{Hofmann:2001bi}. Therefore, $N\approx \sqrt{2/3}\,m_{\nue}/T$ collisions are required to maintain kinetic equilibrium so, when the neutralino is non-relativistic, the temperature of kinetic decoupling is found from solving $\Gamma_{\rm{kd}}=H$, where
\begin{equation}
\Gamma_{\rm{kd}}=\sqrt{\frac{3}{2}}\frac{T}{m_{\nue}}\langle \sigma_{\nue e} v\rangle n_e\;.
\end{equation}

In the limit that the electron mass is zero and left- and right-handed selectrons are degenerate, the thermally averaged elastic scattering cross-section is
\begin{equation}
\langle \sigma_{\nue e} v\rangle=\frac{51}{2 \pi}\left(\frac{m_Z}{m_{\tilde{e}}}\right)^4 G_F^2 \sin^4\theta_W \langle E_e^2\rangle\;,
\end{equation}
where $\langle E_e^2\rangle=12.9 \,T^2$.
With this result, we find that the neutralino drops out of kinetic equilibrium with the electrons when
\begin{equation}
T_{\rm{kd}-e}\approx 2.3 \text{ MeV} \left(\frac{m_{\nue}}{10~\text{MeV}} \right)^{1/4} \left(\frac{m_{\tilde{e}}}{93~\text{GeV}} \right)\;.
\end{equation}
With a more accurate numerical calculation that includes a non-zero electron mass and a thermal average over Fermi-Dirac distributions for the electron and neutralino, we find that $m_{\tilde{e}}>70~\text{GeV}$ for $m_{\nue}=10~\text{MeV}$ in order that $T_{\rm{kd}-e}>2.3~\text{MeV}$. After imposing the ATLAS limit \mbox{$m_{\tilde{e}}>195$~GeV}~\cite{Aad:2012pxa}, we see that the neutralino drops out of kinetic equilibrium with the electrons well before the neutrinos decouple at $T_{\rm{D}}\approx2.3$~MeV.

The sneutrino is kept in equilibrium with the electrons through $Z$- and chargino-exchange. The chargino contribution is smaller than the $Z$-contribution if $m_{\tilde{\chi}_1^{\pm}}>102$~GeV (this assumes the chargino is wino-like to maximise its coupling to the sneutrino, and that the sneutrino has one-third electron flavour). Considering only the $Z$-contribution and ignoring the electron mass we find
\begin{equation}
\langle \sigma_{\tnu e} v\rangle=\frac{\sin^4\theta G_F^2}{\pi}\left(8 \sin\theta_W^4-4 \sin\theta_W^2+1 \right)\langle E_e^2\rangle.
\end{equation}
In this case, the sneutrino drops out of kinetic equilibrium with the electrons when
\begin{equation}
T_{\rm{kd}-e}\approx 2.3 \text{ MeV} \left(\frac{m_{\tnu}}{20~\text{MeV}} \right)^{1/4} \left(\frac{0.37}{\sin\theta} \right)\;.
\end{equation}
Performing a numerical calculation with a non-zero electron mass and a thermal average over Fermi-Dirac distributions for the electron and sneutrino, we also find that $\sin\theta<0.37$ for $m_{\tnu}=20$~MeV. This value of $\sin \theta$ is well above the values we consider, which implies that the sneutrino, like the neutralino, drops out of kinetic equilibrium with the electrons well before the neutrinos decouple.

\section{Conclusions}

In this article we have used the recent Planck measurement of $\Neff$ to set a lower bound on the mass of cold thermal dark matter. These bounds are summarised in eqs.~\eqref{eq:nu_RScalarBound} to~\eqref{eq:nu_DirFermBound} for the case when dark matter is kept in thermal equilibrium with neutrinos and eqs.~\eqref{eq:e_RScalarBound} to~\eqref{eq:e_DirFermBound} for the case when dark matter is kept in thermal equilibrium with electrons and photons. These bounds apply for both $s$- or $p$-wave annihilation cross-sections and are stronger than bounds that can be derived from Big Bang Nucleosynthesis (see table~\ref{tab:bounds}). These bounds apply to models already in the literature such as~\cite{Boehm:2003bt,Ahn:2005ck,Hooper:2008im,Bagnasco:1993st, Pospelov:2000bq,Sigurdson:2004zp,Masso:2009mu, An:2010kc, Fitzpatrick:2010br,2012arXiv1211.0503H} where dark matter annihilates into electrons and could be relevant for models which give a signal at electron recoil direct detection experiments.

The case where the dark matter remains in equilibrium with neutrinos has received less attention so we have constructed a supersymmetric model to realise this scenario. In this model the dark matter is a light bino-like neutralino and it is kept in equilibrium with neutrinos via a mixed left-right handed sneutrino mediator (see fig.~\ref{fig:spectrum}). In the presence of a such a mediator it is possible to achieve the correct relic density (see fig.~\ref{fig:relicabundance}), leading to changes in $\Neff$ (see fig.~\ref{fig:bound}). The Planck measurement of $\Neff$ leads to a lower bound of 3.5~MeV on the neutralino mass in this scenario.

Our bounds may be evaded if the dark matter's abundance has a non-thermal origin (for example asymmetric dark matter), or if the dark matter is in thermal equilibrium with electrons, neutrinos and photons (in which case there is no change in the standard neutrino-photon temperature ratio). Finally, if the dark matter is in thermal equilibrium with electrons and photons and there is also some `dark radiation' such as sterile neutrinos present, the bounds may be weakened.

\section*{Acknowledgements}

We thank Felix Kahlhoefer, Matthew McCullough, Ian Shoemaker, John March-Russell and Stephen West for discussions. MD and CM also wish to thank Michael Spannowsky for `stimulating' discussions. We thank Gary Steigman for pointing out an error in eq.~\eqref{eq:Neff4} in an early version of this work.

redpajama_set_name: RedPajamaArXiv


Prince Harry and Meghan Markle are practicing their baby skills!
After attending a traditional week and luncheon to kick off the final day of their royal tour on Wednesday, local time, the pair headed to Rainbow Springs to learn about the center's kiwi breeding initiative. Kiwis, which are New Zealand's national bird, have become increasingly endangered in recent years, as most Chicks struggle to survive in the wild.
During the royal couple's outing in Melbourne, Australia, the couple hopped on one of the city's iconic trams for a short ride to South Melbourne Beach with student sustainability leaders. Meghan and Harry on a name for the royal baby.
Meghan kept mum, replying, "We've been given a long list of names from everyone, we're going to sit down and have a look at them . "
However, Harry was a bit more open when it came to their new addition. A video posted by the Instagram fan account, Harry_Meghan_Updates, shows a fan calling out to Harry that she hopes the baby "is a girl," and Harry immediately responds, "So do I!" As he continues to walk along the bike path.
Meanwhile, Harry changed from a gray suit into khaki slacks and a black button-up.
Can not get enough of PEOPLE's Royals coverage? Kate Middleton, Meghan Markle and more!
The royal couple are just starting their royal journey – with some adorable animals! They spent their first day in Sydney, where they visited the Taronga Zoo.
Meghan and Harry were also introduced to a yellow-bellied glider, a type of native possum, and Lynx, a short-legged echidna.
RELATED VIDEO: Prince Harry and Meghan Markle Kick Off Their First Royal Tour in Sydney [What's wrong?] 19659025] The whirlwind 16-day tour Down Under in Sydney, with a number of day trips to other areas of the country, and kicked off the 2018 Invictus Games before spending a few days in Fiji and Tonga.
They returned to Sydney for the end of the Invictus Games before heading to New Zealand to wrap up their tour.


text:
Some Nights (en español: Algunas noches) es el segundo álbum de estudio de la banda de rock alternativo e indie pop, Fun.. Fue lanzado el 21 de febrero de 2012 por Fueled by Ramen. Fue grabado en el 2011 y producido por Jeff Bhasker. Después de firmar con un nuevo sello, la banda comenzó a trabajar en Some Nights durante más de nueve meses.

«We Are Young» fue lanzado como el primer sencillo del álbum y reforzó el éxito de la banda con la ayuda de la televisión y la publicidad. Subió rápidamente en los EE. UU. En la lista Billboard Hot 100 estuvo durante seis semanas en el puesto número uno y en Alternative Songs durante dos semanas, con más de tres millones de descargas digitales. La canción « Some Nights» fue comisionada como su segundo sencillo, alcanzó el puesto número tres en el Billboard Hot 100, además de convertirse en su segundo número uno en Alternative Songs. El álbum recibió críticas positivas según Metacritic.

Orígenes
La banda firmó con Fueled by Ramen a finales de 2010. El vocalista Nate Ruess, que tenía temores acerca de unirse a un sello importante anteriormente, recordó la formación «muy, muy fácil» del grupo, indicando que todos se agruparon como si «supieran exactamente lo que hacían». Casi nueve meses duró la transición de Fun. con la discográfíca para empezar a trabajar, ahí fue cuando el titular de la discográfica se acercó a la banda. Ruess se sintió halagado de que los empleados del sello iban a comprar sus propios entradas para poder ver el espectáculo de Fun. y «hablar de nosotros con la pasión que generalmente estaba reservada para un artista que está trabajando con ellos». Después de largas discusiones dentro de la banda, la banda decidió dar una oportunidad a la discográfica.

Ruess recuerda que él estaba escuchando «mucho hip-hop», durante la producción, que se convirtió en una gran influencia para él. La banda se sintió inspirada y poco a poco comenzaron a trabajar en nuevas canciones, cada uno con una evidente influencia del hip-hop. Conscientemente, la banda trabajó en el factor de hip-hop y se dieron cuenta de que querían un productor de hip-hop. Después de repasar los créditos de sus propios discos de hip-hop, Ruess se dio cuenta de que Jeff Bhasker era uno de los nombres que más se repetían. Bhasker estaba ocupado con un trabajo con Beyoncé, pero Ruess fue insistente al reunirse con él.

Grabación y producción
El proceso creativo más común en la grabación de Some Nights se inició con Ruess. Ruess venía con una letra y la melodía, lo que lleva a Andrew Dost y el guitarrista Jack Antonoff a construir la estructura de acordes y la instrumentación, o «el apoyo de la melodía». Dost señaló que en la grabación, a pesar de un bien definido marco del compositor, los egos de los individuos «casi desaparecieron» y «todo el mundo estaba feliz de trabajar en la mejor canción posible» coherentemente entre sí. La dinámica entre Bhasker y la banda en el estudio fue inspirado mutuamente, como Bhasker nunca había trabajado con un grupo de rock antes y diversión. Nunca había trabajado con un productor de hip-hop. Bhasker particular disfrutamos de las guitarras de grabación con el guitarrista Jack Antonoff como no estaba acostumbrado a ella, y sintió Dost audición componer beats Bhasker fue «alucinante».

El énfasis para Ruess en algunas noches era hacer las canciones más cohesionada, mientras sentía que su escritura era "por todas partes". Esto significó la creación de canciones que eran concisas en vez de ser "largo y prolongado". Bhasker era un defensor de la utilización de un único instrumento para proporcionar los mayores ruidos, deseando no a "sobre-meter [las] canciones con las ideas" declarando que todo lo que hace que la canción debe ser bien elegido. Janelle Monáe colaborado con el trío de "We Are Young" a través de una amistad con Bhasker. Bhasker fue acreditado con traer a la banda un sonido más grande y completo de un traducción sonic nuevo a la banda no está presente en su debut, Aim e Ignite.
El álbum se crea una mezcla de pop indie, rock teatral, y hip-hop, un sonido que se le atribuye a Bhasker. Algunas noches como un título flotaba alrededor antes de las canciones del álbum fueron creadas uniforme y fue concebido por Reuss. Fue inspirado por la forma en personalidades pueden cambiar en cualquier noche dada. Aunque el álbum no es un álbum conceptual, el título cambió las ideas de la banda para el álbum considerablemente, con Dost diciendo: "Es muy agradable una vez que tenga un título para saber cuáles son los parámetros de lo que usted está trabajando en su conjunto ". La banda terminó la producción en el álbum en octubre de 2011. Ruess llamado los siete meses que pasó grabar el disco el más gratificante de todo en sus diez años de trabajo profesional de música, llamándolo su punto culminante carrera.

Composición
El álbum y la música de la banda ha recibido varias comparaciones a Queen. Rolling Stones's Jody Rosen, llamado el álbum una mezcla de "corales estrecha armonía y vistosas cambios clave, una pizca de Queen aquí, una cucharada de Les Miz allí ". Marcus Glimer de The AV Club escribió que el álbum contó con más "elementos sintéticos [más teclados y baterías electrónicas]" que su álbum debut, AIM e Ignite y comparó el ritmo de "All Alone" en una pista de hip-hop. NPR columnista Daoud Tyler-Amin comentó que el álbum podría ser el comienzo de una nueva etapa de la música, en el que los músicos que infundir los sonidos y ritmos "una vez asociados con el hip- hop "con su música pop.

Letras de canciones del álbum han sido llamados "quejumbrosa", para tratar temas de la soledad, la autoestima, la introspección, la paranoia y el existencialismo, en contraste con el "himno" del álbum de música. Tyler-Ameen considerado el álbum "notable por su optimismo puro ", a pesar de las letras tristes y lúgubres. Reuss don para el himno se corresponde con Gen-Y humor Rosen escribió que "- emo auto-desprecio que hace fermentar la ampulosidad". Reuss tarde comentó sobre la importancia de las letras a él, diciendo que él tomó "un gran orgullo", después de que terminó de escribir ellos. Asimismo, consideró la mayoría de letras escritas por músicos actuales que hay que "disminuidos", parcialmente causar "problemas actuales de la escena del rock".

Lista de canciones

Videografía
 We Are Young (Con Janelle Monáe)
 Some Nights Intro (Video No Promocional)
 Some Nights
 Carry On
 Why Am I the One
 One Foot (Video Promocional)

Certificaciones

Referencias

Álbumes de 2012
Álbumes certificados de platino por la Australian Recording Industry Association
Álbumes certificados de platino por la Irish Recorded Music Association
Álbumes certificados de platino por la Recording Industry Association of New Zealand
Álbumes certificados de platino por la British Phonographic Industry
Álbumes certificados de platino por la Recording Industry Association of America
Álbumes certificados de oro por la Recording Industry Association of Japan
Álbumes certificados de oro por la Grammofonleverantörernas förening

redpajama_set_name: RedPajamaWikipedia


text:
Developer Chooses CFS Steel Over Wood, Cites Speed
By choosing cold-formed steel (CFS) for the project, Augustine tapped into both the versatility and durability that are unique qualities of the product, which enabled them to maximize its use for 34,000 linear feet of non-load bearing (nonstructural) CFS walls and 38,000 linear feet of prefabricated load-bearing (structural) CFS walls
Westervelt to Build 250 Mbf Lumber Mill in Alabama
Tuscaloosa's Westervelt Co. says it is completing plans for a new lumber facility in south Alabama which is expected to employ about 100 people.
WTO Appoints Two Panels to Investigate Lumber Tariffs
The World Trade Organization says its dispute settlement body has agreed to establish two panels to examine Canada's complaint about duties imposed by the United States on softwood lumber imports.
BC Lumber Exports to U.S. Down 20%, Rail to Blame?
Softwood lumber exports from British Columbia to the United States plunged 20 per cent in March from a year ago, the federal government said, amid railway transportation problems.
Charts: Building Material Costs Continue to Rise
Building material costs continues to increase, according to the U.S. Bureau of Labor Statistics' recent Producer Price Index report, and many are looking at ongoing trade disputes as a big part of the problem.
Consider Costs of Steel Uncertainty, and Pass Them On?
Just over a month after the Trump Administration announced it was going to place tariffs on imported steel and aluminum, we are beginning to see bilateral agreements and renegotiated trade deals taking place.
As Lumber Costs Soar, Where is the Demand?
Lumber costs are often thought to be controlled by simple supply and demand. We've recently published several articles addressing the supply side of this equation, but what about demand?
Steel Industry Focuses on Fire Performance Versus Wood
Steel has an obvious advantage in that its core ingredients are fire resistant. So, that begs the question that shouldn't more steel structures be speced and built?
Infographic: Prefabricated CFS Components Gaining Traction
Cold-formed steel (CFS) framing, for instance, is an ideal choice because it is non-combustible, lightweight, and cut to precise specifications. Learn more about the benefits of prefabrication and CFS by exploring the infographic below.
Canada Escalates Lumber Dispute Through WTO Request
Canada plans to ask the World Trade Organization (WTO) to set up an adjudication panel to judge its dispute with the United States over Canadian lumber exports, indicating that talks have failed to resolve the issue and Ottawa is pressing its case.


text:
Category Archives: Play
23rd Discussion: Eleanor Wong's Invitation to Treat (17 Aug)
Li Sian and Raj were against the rest of us. Li Sian argued there is a general development of the trilogy from the personal coming out to themes such as kinship and religion and finally to building a lesbian community. There is a political awakening in each of the three plays. Both Jason and Davina liked Wills & Secession for the issues being brought up and because Grace is the only character Davina could identify with. Javin thought that the plays are preachy and self-righteous and the characters don't have psychology behind them.
1. Themes:
a. Class: One reason why Davina couldn't identify with the trilogy is that the lesbians are all middle-higher class earners. It seems that, Aaron argued, to be lesbian in Singapore, one has to be successful or risk non-representation. Alex reminded us that these are plays, written for a relatively exclusive class of people. Davina then continued that these are "dangerous" plays. What if this were the one book she turned to to find out the lesbian existence in Singapore? The plays would easily fall into the stereotype that homosexuality is a rich person's "disease." The poor can't be gay. Feeding on Davina's idea, Aaron said that the opposite is true, that is money is used to glamorize lesbianism and indeed why such insecurity, and such overcompensation? On the other hand, Li Sian reasoned that it is unreasonable that we shouldn't expect activistic work from the plays; and Timmy commented that Wong is only writing the world she knows. Raj, while defending the play, called it "self-centred" but so what? Aaron noted then that if Wong is only writing for herself, then she's "self-centred," why do we read her? If she is writing for others, to be performed as plays, then she fails to represent lesbians probably.
b. Religion: Li Sian provided us with the statistics that 35% of the highest earners are Christians and 50% of the politicians on a *er-hum* certain country are Christians. So when they speak in Parliament, their morality stems from their high class status and their religion, very out of touch with the society.
c. Men: Jason pointed out that all men are depicted as assholes, especially Grace's husband. Timmy further observed even the one gay man is stereotypical, acting as comical relief and perfidious. Li Sian defended the writing that at least the men are complex and interesting.
d. Women: Raj notes that the lesbians are all strong woman characters but Aaron pondered over the lack of representation.
e. Politics: Li Sian very astutely noticed that the personal is political where it comes to Ellen although Javin found the message to be propagandistic and preachy.
f. Love/ Relationship: Raj noted the parallel image of a 3-way relationship in the first and last play. Li Sian saw the acceptance of a threesome as queer. Isaac suggested that the plays are about opening spaces of possibilities, including the possibility of a 3-way relationship. Jason, however, brought up the line that resonates throughout the plays, that is, there is no rule book for lesbians but he contended that there surely must be, such as respect for each other.
2. Characters:
a. Ellen: Lots of conspiracy theories revolving Ellen. Timmy claimed Ellen makes use of Jon. Li Sian thought it was a marriage of convenience. Javin believed that Ellen takes a stab at normalcy and Raj conjectured that Ellen is tired of failed lesbian relationships and she's filling up the gap left by her parents. Li Sian has much respect for Ellen as "she changed my life." Ellen is radical as a gay icon, Li Sian argued convincingly, because Ellen has a child, lives her life as she wants–honestly–while doing activist work. Aaron wondered if Ellen's first world problems are trivial because the problems portray a very selfish, egoistic and narrow-minded self. Even Isaac, known for his beneficence, agreed that although Wong is writing on a universal issue, she presents it such that few people could identify with it. Li Sian rightly countered that first world problems are problems too. Jason chipped that although Ellen is flawed and egoistic, it is what makes her human. Aaron further claimed that Ellen has no personal development. In each play, she makes the same kind of mistakes over and over again. When will she ever learn? When will she grow? Raj alleged that perhaps it's Ellen's personality, so why can't she make the mistake over and over again?
b. Sam: Jason pitied Sam for her parentage although Li Sian said that from experience children from divorced families are happier than from families in which parents stay together in an unhappy state. Aaron said that Sam grows up sane and successful to prove a point, of course, that lesbians can make good mothers.
c. Grace: The naming of "Grace" is important, Jason noted, since it is the cause of Ellen's overcompensation and her attitude towards her parents. Li Sian liked how Grace proves that a Christian can also be accepting of homosexuality, can be a good person and a good sister. Javin jumped in, saying that Grace as an exemplar is propagandistic.
As we concluded the session, no side could convince the other. Raj still liked the plays, just because. Like a true blue diva. Li Sian still liked it because it has everything, from the political to existential cycle of being gay. Timmy was still on the fence, saying that the plays are about being human. Being diplomatic, Jason said it is thought-provoking and Davina said it is a starting point for Singapore lesbian literature. Alex hated the mawkishness of it; Isaac thought that although the book is on a universal theme, not many can identify with it; Javin believed it was trying too hard to persuade and convince the audience to accept homosexuals. Having watched the performance, Aaron was at first partial to the plays but as the discussion went on, he had a nagging feeling the plays were elitist and the characters are very unlikeable.
Filed under Bisexuality, Class, Eleanor Wong, Family, Lesbian, Love, Play, Politics, Religion, Singapore


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Visit us at The Kensington to pick up your bracelet. Then, spread the word…and the love.
You can also follow @TheKensingtonFC on Twitter for updates, industry advances and current news surrounding the fight against Alzheimer's.
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Massless, teamLab's first exhibition in the Nordic countries of Europe, celebrates the transformation of Helsinki's Amos Anderson Art Museum into Amos Rex by filling the majority of the institution's newly minted subterranean home with a series of immersive, multimedia installations. Curated by museum director Kai Kartio and comprising five recent digital animations, the Japanese art collective's mandate is to deprive art of its material qualities. Out of necessity, it also forces visitors to proceed hesitantly when navigating the pitch-black passageways leading from one installation to the next. This engenders a profound sense of relief in addition to immense surprise and delight when discovering the inimitable simulated environments that fill the museum's galleries.
The one exception to this, however, is 'Enso' (2017), an inherently beautiful series of calligraphic brush strokes that splash onto a large wall mounted screen, which greets the viewer in the bright and spacious entrance hall. These splatters of digital ink, applied with an invisible brush, are never still. Floating in a shallow space, they slowly drift or rotate. At times, they grow ever more viscous and ink appears to drip from the edges. Wisps of dark vapour will rise into the space around them and much more solid-looking splinters of colour are also discharged and occasionally, a new brush stroke will be applied over an existing mark. The latter's tones will lighten and become increasingly transparent until no visible traces remains.
This ode to fluidity is reprised and greatly magnified in 'Black Waves' (2016), a black, blue and white, primarily linear composition depicting a surging flow of water that is robust, visually alluring, ongoing and, in tandem with Hideaki Takahashi's sound track, entrancingly meditative. Moreover, it recalls Hokusai's formulaic and decidedly illustrative style of rendering, principally his famous 'Kanagawa oki nami-ura' (c. 1829 - 1833). Unfortunately, the chromatically related and site specific 'Vortex of Light Particles' (2018) fails to make an equally impressive impact. Located in the museum's great domed space, it was intended to be the exhibition's high point, but the ceiling's pattern subverts the water's flow. Moreover, the location of the giant black hole that is its destination, feels stilted. The walls that border the room also come across like an ill-fitting skirt. The heavy use of organ in the sound track adds an unwelcome churchy-ness. Though the potential of the concept is clearly evident, its realisation has not lived up it, and that is deeply disappointing.
In contrast, 'Graffiti Nature: Lost, Immersed and Reborn' (2017), is very arresting. The activity level of what can become a franticly exotic garden relies on visitors' input, and of that there is plenty. Without it, the plants and animals that occupy it fade away. Rubbing one's hand on a blank wall will, for example, counter this. The gesture will cause flowers to burst forth and butterflies to appear. Stomping on animals creates short lived splatters of paint to show up on the floor. Step on them too often and they expire. Anyone can also contribute to this ecosystem by colouring some of the preprinted animal line drawings. Once scanned, their creatures join the system's population. But, as engaging as this installation is, the actions of rubbing and stomping soon lose their appeal. Interestingly, the most absorbing process involves participating in the work, which, to a degree, also sidesteps teamLab's mandate. The desire to deprive art of its material qualities, even though the hand coloured images are not shown, is not completely realised. Participants cross a line; unlike viewers' relationships to other works in the exhibition, here they do not remain mere observers. The process encompasses a modicum of personal freedom to affect the proceedings as well as haptic sensory experiences, at least to a degree.
In my mind, 'Crows are Chased and the Chasing Crows are Destined to be Chased as well, Transcending Space' (2017), closes the presentation on a high note. This short, 4 min 20 sec long work takes in all surfaces of the otherwise empty shoe box-like shaped room. It begins with a flash of light and the sound of a gong, and then the static images wrapping the space begin to move and create the very realistic feeling that viewers and/or the space are tilting and turning. This appeals to fans of roller coasters, but risks making others feel nauseous. Soon, it seems we are zipping through the atmosphere with mythical Asian three-legged crows, as the action intensifies, the music also crescendos. It becomes impossible to see everything in this 360º work. Eventually flowers emerge. Petals are set adrift. Soon after forms suggestive of asteroids appear and the sound and motion begin to subside.
The accompanying guide states that the piece refers to the cyclical nature of life and the natural world's transient nature. It is driven by a computer program and plays in real time. The sequences change with each performance and no two performances are the same. But does one need to be aware of these facts? Not really. Though correspondences to the other installations are evident, one can simply soak up the visuals, enjoy the soundtrack and go back a second or a third time to experience it again and again. It is very dream-like and, as is the case with dreams, much of what transpires eludes precise verbal description.


However, if the computer is a laptop and you use other networks aside from your business's service, choose "Public network." If you use an air card to connect to a mobile broadband carrier... 10/09/2015 · Second, your screenshot shows the other MS accounts of yours, which can be added to your user account in Settings > Your account > Other accounts you use. These accounts may but they don't need to be added as user accounts on you computer.
So you can't truly clean up a profile by simply deleting a user's files. Although checking the total usage of C:\Users can be helpful when looking to free up some disk space. You can use Windows explorer and examine properties as I do in Figure 1.
Another approach you can take to purge old profiles is to use Windows PowerShell and Windows Management Instrumentation (WMI). The Win32_UserProfile class is the place to start. The Win32_UserProfile class is the place to start.