Showing posts with label ENGL. Show all posts
Showing posts with label ENGL. Show all posts

Monday, January 26, 2015

The Century of Strong Gravity

The following is a popular science article that Richard, Vitor and I have written for the IST Physics Magazine "Pulsar" (here is the Facebook page) and that will also appear in the Portuguese Physics Magazine "Gazeta de Fisica". A pdf version is available here (in English), and here (in Portuguese).





1. One Hundred Years of Gravity

The latest Christopher Nolan's movie, Interstellar, is about a future human civilization able to undertake cosmic travels to black holes using special shortcuts, ``wormholes''. Science-fiction as it might seem, Interstellar screenplayers --who happen to be the Nolan brothers-- have worked side by side with Kip Thorne, a professor of Theoretical Physics at the California Institute of Technology and one of the fathers of modern General Relativity, the theory that explains what wormholes and black holes are and how they form in the Universe.

Thorne's contribution is to ensure that the movie --starring Matthew McConaughey and Anne Hathaway among others-- doesn't contain scenes that would make Albert Einstein cringe.
Does this mean that travel agencies are about to sell (roundtrip!) tickets to a black hole? Not quite, but in a few years from now, theoretical physicists and astronomers will be able to study them as never before. The scientific payoff of these studies will largely overcome Interstellar's box-office, with all due respect to Mr. Nolan!


Saturday, January 17, 2015

Visit to AEI

This week I was visiting the Max Planck Institute for Gravitational Physics (aka Albert Einstein Institute, AEI) in Golm, in the outskirts of Potsdam, in the outskirts of Berlin (this more or less reflects the number of connections that commuters living in Berlin have to take everyday). The location of the institute is really its only weakness because otherwise the place looks great.

Jan and I taking a selfie with Albert. The statue is located at the middle of a beautiful large indoor yard 
at the Albert Einstein Institute in Potsdam (Germany)

I was there to collaborate with Jan Steinhoff (see pic above) who was postdoc in Lisbon in the last few years and recently moved to the AEI to work in gravitational-wave group lead by the new Director of the institute, Prof. Alessandra Buonanno, a world-leading expert in gravitational-wave phenomenology (and also one of the key speakers of this upcoming workshop). While there, I gave a seminar on "Black holes as stong-gravity labs", presenting some recent results related to black-hole superradiance (a topic that I will cover in this blog soon). I've also took the opportunity to discuss with a lot of interesting people working at the AEI (and to have some German beers with Jan and Jordi Casanellas, who also moved to AEI from Lisbon).

Sunday, January 4, 2015

Workshop: "Compact Objects as Astrophysical and Gravitational Probes" at the Lorentz Center (Feb 2-6, 2015)

It's a pleasure to advertise the workshop  "Compact Objects as Astrophysical and Gravitational Probes", to be held at the Lorentz Center (Leiden, The Netherlands) from February 2 through February 6.

One version of the workshop's poster, the official one will soon appear in the official webpage.
Here young Subrahmanyan Chandrasekhar and Albert Einstein are looking towards the most urgent questions in relativistic astrophysics, a field that has essentially emerged from their seminal works. The two young guys respectively symbolize the astrophysical and the general-relativistic communities that will gather together at this workshop, to share expertize and try to fill the gap between them
.
Last June, Enrico Barausse (at the Institut Astrophysique de Paris), Tamara Bogdanovic (at Georgia Tech in Atlanta), Vitor Cardoso (at CENTRA - Instituto Superior Tecnico in Lisbon) and Elena Maria Rossi (at Leiden University in the Netherlands) and myself have applied to an international call at the Lorentz Center to organize a workshop. We initially had in mind a small-size workshop with ~20 participants, but the proposal was selected for a large-size event. Thus, in less than one month, more than 50 world-leading experts in relativistic astrophysics will gather together in what will hopefully be a fruitful and exciting meeting (here is the program and at list of participants).


Wednesday, December 10, 2014

Recommended by us: Interview with John Ellis



To come across John Ellis at CERN is actually not a rare event: at seminars, at coffee breaks... But probably in those situations you do not have so much courage or time to ask him what is his position about the role of science in the society, or even more when he decided to become a theoretical physicist!

If you have a kind of curiosity about these topics and other related questions, take a look at this interview: past CERN Summer Students with the kind help of the PH Newsletter have had the fortune to ask to him directly

http://ph-news.web.cern.ch/content/interview-john-ellis


Have a good read and, if you will have the patience to go until the end, you will find a final question to you.

Saturday, December 6, 2014

Pre-celeberating 2015 for 100 years of Einstein's General Relativity and maybe more...


In a few weeks we will all land in the exciting year of 2015! Many people will be celebrating New Year, as usual! (but still exciting) But, unusually, gravity physicists will be celebrating 100 years of General Relativity after Albert Einstein. 

in 2015, gravitational-wave physicists, although, may have one extra celebration to do on the top of others, which is celebrating the first direct detection of gravitational waves! Advanced version of gravitational-wave detectors will start to take data in a few month, hunting wild celestial gravitational-wave sources such as black-holes and neutron-stars. I'll write more about this here some time soon. But for now, you may check out my earlier post in Gravity Room.


Anyways, just before entering in to 2015, Princeton University has recently released The Digital Einstein Papers in an open-access website which is an awesome collection and an excellent holiday reading! All the papers are in both English and German languages.




Friday, October 24, 2014

Tullio Regge passed away

Tullio Regge (July 11, 1931 in Turin - October 23, 2014 in Orbassano)

Theoretical physicist and mathematician Tullio Regge, aged 83, passed away yesterday. He gave fundamental contributions to scattering theory (the theory of Regge poles is named after him) and to General Relativity among many other fields. His "Regge calculus" -based on a discretization of spacetime- is still widely used in Loop Quantum Gravity.

The relevance of Regge's heritage in modern physics is well shown by the fact that something like half of my papers cite the so-called Regge-Wheeler equation which describes how a Schwarzschild black hole vibrates after a perturbation and how it emits gravitational waves. The Regge-Wheeler equation was found in the late 1950s, even before the very concept of "black hole" (a name coined by Wheeler only in the 1960s) was formulated.

The Italian Institute for Nuclear Physics has dedicated its homepage to this news, more details on Regge's work can be found here.

Friday, October 17, 2014

The brightest pulsar ever

Last week the astrophysics community was hit by an exciting news. A very luminous X-ray source located in the "Cigar" galaxy M82 was discovered to be a spinning neutron star (a pulsar) rather than a black hole, as all models have assumed so far. This research was lead by astrophysicist Matteo Bachetti, who also happens to be a writer of this blog. Thus, we take the opportunity to ask Matteo a couple of questions whose answers you will not find in the excellent press (and radio) coverage that has followed the publication of this discovery.




Q: Matteo, first of all congratulations for what sounds like a great scientific achievement! How would you explain this discovery to my grandma? 


Thursday, September 18, 2014

Running Citizenship

Today's historical referendum in Scotland gives me the opportunity to talk about something I have in mind since I came back from the U.S. earlier this year. It's actually a very trivial concept that originates from the fact that:

When outside Europe, I feel European. When within Europe, I feel Southern European/ Mediterranean. When in Southern Europe, I feel Italian and, finally, when in Italy I definitely feel Sardinian. 

There is actually no contradiction in this Matrioska-like sense of belonging and I'm sure most people who happen to live abroad (which is already a rather subjective concept....) share the same feeling.

Anyway, this is interesting because in physics there is a much deeper and far-reaching concept that is (vaguely) related to the one above: that of the running couplings. In a quantum field theory, the coupling "constants" that define the strength of the couplings among quantum fields are not really constant, but actually their values depend on the energy scales.

As an example, take the most famous coupling constant, Newton's gravitational constant G that appears in the gravitational force law

F= G*mass1*mass2 / distance^2

which simply means that the intensity of the gravitational force between two masses (mass1 and mass2) is proportional to the masses and inversely proportional to the square of the distance. The proportionality factor is nothing but what we use to call Newton's constant and its value is G~6.673×10^{-11} N·(m/kg)^2. Now, Newtonian gravity is a classical theory and there is no such thing like a running G (although the situation might be different in alternative theories of gravity, such as scalar-tensor theories, but this is another story...). Indeed, G is a constant no matter how close the two masses are or how massive the objects are. In a quantum field theory, G would depend on the energy involved, for example on the typical distance of the interaction.

If you think about that, this is a beautiful and elegant concept: it teaches us there's no such thing like "the ultimate theory", but each theory (if consistently quantized) would be different at different energy scales. For example, a theory like electromagnetism (or QED in its quantum version) becomes more strongly coupled as the energy increases. The QED coupling constant (the fine structure constant α) is about α ≈ 1/137 at low energies, whereas one measures α ≈ 1/127 at the scale of the Z boson, about 90 GeV. A theory like quantum chromodynamics (QCD) behaves exactly in the opposite way and it becomes more weakly coupled at high energies. This phenomenon is called asymptotic freedom (because the interaction between particles becomes zero at infinite energy) and its discovery  (by Frank Wilczek, David Gross and David Politzer) was worth the Nobel prize in 2004.

What does this have to do with Scotland? (if anything...) The idea that can be borrowed from particle physics is that of a "running citizenship". In other words, each person changes her/his sense of belonging to some country/community accordingly to the "characteristic scale of the problem". It's something that European people are already experiencing given that economy in Europe is mainly governed on European scales, whereas local regulations are governed by state laws. Something similar also happens for federal countries, although the idea of running citizenship that i'm trying to describe has more to do with sense of belonging than with politics (politics often tries to change the sense of belonging and to tailor it accordingly, though).

In physics, the theory that studies the running couplings is called renormalization group and the running is usually called "flow". In most theories, the coupling either grows or decreases with energy, but for some special theories it asymptotes a constant value, a "fixed point".

As for the running citizenship, my impression is that we better try to have a fixed point for that, because the other two cases are quite catastrophic. The analog of a theory like QED would be a sense of citizenship that becomes smaller and smaller as smaller scales are approached, eventually terminating in individuals that do not belong any community. This would imply a sort of total isolation for each individual. The other case would be funny: an individual would become more and more aware of the global nature of Mankind and would feel like more and more part of the entire Universe as smaller scales are approached (this sounds like a nice outcome but perhaps a bit too Hippie for these times....). The most natural solution would be approaching a limit, a minimum size of the community (which we can perhaps identify with the family or hopefully with something larger than that) and then having each person feeling as a part of a larger community dependending on the context and the environment.

In which category does the running citizenship flow of the Scottish people fall? We shall discover this quite soon and the outcome has probably very little to do with physics.....


Tuesday, July 22, 2014

Jordi on Dark Matter @ FameLab 2014

Fame Lab is a competition to find new voices of science across the world. In these events various speakers compete for the best popular science short talk. The events are hosted in various countries and there are competitions at regional, national and international level.

This year Jordi Casanellas (former PhD student in IST-Lisbon and now postdoc at the Albert Einstein Institute near Berlin) attended Fame Lab Germany. As the video below shows, in the first stages of the competition speakers cannot use blackboards (not to mention slides or projectors) and their talk has to be ~3 mins long.



Jordi talked about his field of research, Dark Matter, and in fact did a great job: he passed the regional competition and went to the national finals (see video below), where he placed second!




So, if you want to have an idea of what Dark Matter exactly is (or what scientists actually think it should be...) you don't have to do anything but listen to Jordi's speeches. Enjoy!

Sunday, July 13, 2014

Pull back: "Scientist: Four golden lessons" by Steven Weinberg

Just came across this brilliant essay by Nobel Laureate Steven Weinberg, writing about his experience as a young scholar, his first steps in research and the connection between science and epistemology.



The essay is so short and clear that I could have copied it here in its entirety, but I'll just give you one inspirational paragraph:

[...]
Look back 100 years, to 1903. How important is it now who was Prime Minister of Great Britain in 1903, or President of the United States? What stands out as really important is that at McGill University, Ernest Rutherford and Frederick Soddy were working out the nature of radioactivity. This work (of course!) had practical applications, but much more important were its cultural implications. 
[...]

and leave the rest for the original

Wednesday, June 4, 2014

"Science in the era of Facebook and Twitter – get used to it" by Heino Falcke

Astronomer Heino Falcke has recently wrote a nice post on the relation between science, dissemination of scientific results and social media.

The post was triggered by the recent debate on the BICEP2 results and contains interesting advices on the new role that scientists and journalists should learn to have in the era of Facebook.

“Science is wrong, most of the time” – I am not sure who said that first, but I am sure someone did so well before me. This is a banality for those who do science at the forefront of our knowledge, yet sometimes it seems very difficult to also accept that view in the public discourse. Well, in the days of Facebook and Twitter it is plain obvious to everyone.


Continue reading on Heino Falcke's blog

Tuesday, May 13, 2014

Recommended by us: "Is BICEP wrong?"

“ 

Blockbuster Big Bang Result May Fizzle, Rumor Suggests


The biggest discovery in cosmology in a decade could turn out to be an experimental artifact—at least according to an Internet rumor. The team that reported the discovery is sticking by its work, however.
Eight weeks ago, researchers working with a specialized telescope at the South Pole reported the observation of pinwheel-like swirls in the polarization of the afterglow of the big bang, or cosmic microwave background (CMB). Those swirls are traces of gravitational waves rippling through the fabric of spacetime a sliver of a second after the big bang, argue researchers working with the Background Imaging of Cosmic Extragalactic Polarization 2 (BICEP2) telescope. Such waves fulfilled a prediction of a wild theory called inflation, which says that in the first 10-32 seconds, the universe underwent a mind-boggling exponential growth spurt. Many scientists hailed the result as a "smoking gun" for inflation.
However, scientists cautioned that the result would have to be scrutinized thoroughly. And now a potential problem with the BICEP analysis has emerged, says Adam Falkowski, a theoretical particle physicist at the Laboratory of Theoretical Physics of Orsay in France and author of the Résonaances blog. The BICEP researchers mapped the polarization of the CMB across a patch of sky measuring 15° by 60°. To study the CMB signal, however, they first had to subtract the "foreground" of microwaves generated by dust within our galaxy, and the BICEP team may have done that incorrectly, Falkowski reports on his blog today.
To subtract the galactic foreground, BICEP researchers relied on a particular map of it generated by the European Space Agency's spacecraft Planck, which mapped the CMB across the entire sky from 2009 until last year. However, the BICEP team apparently interpreted the map as showing only the galactic emissions. In reality, it may also contain the largely unpolarized hazy glow from other galaxies, which has the effect of making the galactic microwaves coming from any particular point of the sky look less thoroughly polarized than they actually are. So using the map to strip out the galactic foreground may actually leave some of that foreground in the data where it could produce a spurious signal, Falkowski explains. "Apparently, there is something that needs to be corrected, so at this point the BICEP result cannot be taken at face value," he tells Science.
Continue to read on Science 



                                                                                                                                                                                          
See also http://resonaances.blogspot.fr/2014/05/is-bicep-wrong.html
     

Thursday, April 24, 2014

The first observed SMBHB?

An artistic illustration of black hole
SMBHB stands for Super Massive Black Hole Binary. If the results get confirmed, this shows that we have observed inactive SMBHBs for the first time ever! SMBHs can be 10^7 times more massive than our own Sun. The Sun is one million times more massive than the Earth. The mass of Earth is about 10^24 kg, by the way.

SMBHBs can be used as excellent natural labs for testing many aspects of gravitational and high-energy physics. As you might know already or might just guess from the term "black hole", a black hole cannot be seen by our usual optical telescopes (not even by other common types of telescopes in other ranges of frequencies of electromagnetic waves such as radio-telescopes and x-ray telescopes). A black hole is such a massive object that even light cannot scape from its gravitational field. That’s also why you can not see a black hole, simply because neither light nor other electromagnetic waves can scape from the gravitational field of a black hole and reach your eyes. The only way to observe black holes is studying their gravitational field effect on the motion of nearby stars. An even better way to study and observe these inconspicuous giants is listening to them! (check out this note to see how) They are pretty loud!

To check out more details about this first serious candidate of SMBHB at the galaxy SDSS J120136.02+300305.5, see the original article, published recently at The Astrophysical Journal: F. K. Liu et al. 2014 ApJ 786 103.

Thursday, April 3, 2014

Listening to Gravitational Waves [1]: a very simple analogy!



Universe is a Jungle and Gravitational Waves are sounds of the animals in it

Close your eyes and imagine you are in a helicopter flying over a very big beautiful jungle in the heart of Africa. Open your eyes now! What you see is like the following pictures: a lot of trees and plants which you see them as a big, green picture and call it “jungle”!

What you see from your helicopter above a huge jungle in Africa

The ground is so covered by trees and plants such that there is no way to see the animals who are living in this jungle from your helicopter flying ~500m above the ground. You also can’t hear their voices. Even though you do believe that lions, tigers, elephants, monkeys, and etc are living down there and make some sounds some times naturally, based of what Mr. Einstein have told you. You have never seen these animals before but according to Mr. Einstein, they should sound like followings: tigers [listen], lions [listen], elephants [listen], monkeys [listen].



There are some animals under the jungle trees that there is no way to see them from your helicopter, you just can hear their voices

However you can not see the lions in the jungle because they have hidden by many trees, but you are able to see if some birds are flying around your helicopter or even very far away, but above the trees.

You are able to see if some birds are flying around your helicopter or even far away, but above the jungle trees.

Unwanted sounds from your helicopter: noises!

Unfortunately, you can not hear any animal voice neither birds nor lions. Noise of your helicopter engine [listen] is the only sound that you can hear (however you probably can hear your friend beside you when he is shouting in your ear). With the assumption of a completely silent helicopter, not all the animals have strong voices which can reach you at the helicopter. Even if the animals make strong enough voices, in reality, what you hear is helicopter noise plus an extremely weak voice of an animal. Therefore it would be so difficult to recognize the animal voice in presence of such a high level of noise. In the best circumstances, you will need a super-duper high-tech artificial ears to filter out animal voice from helicopter noise. To do this, indeed, it will be required to know how does the animal voice that you are looking for look like. You can not use voice of monkey and look for voice of lion in the data! Fortunately, by experience, we do know what does the voice of a typical lion look like, however the African lion voice might be a little different. But it doesn’t matter that much, it perfectly works for our purpose.

In fact, voice, or basically sound wave, is not more than some simple mechanical waves in the air. When you speak, your vocal cords shake the air around and make some mechanical waves in air which can be heard by your friend’s ears. Waves, in all forms, need an environment to travel through. If you speak in vacuum [suppose your body doesn’t implode in vacuum!] nobody can hear you. Gravitational waves, in the other hand, are some kind of waves which are produced by moving super-massive sky-objects like black holes, and neutron stars. Instead of air in the case of sound waves, gravitational waves travel trough the fabric of spacetime and affect masses in the field. Gravitational waves are prediction of Einstein’s general theory of relativity. If strong gravitational waves go through your body, you will experience a situation like the following picture. Although, effects are super exaggerated in this picture. 

When strong gravitational waves go through your body. (different polarization)

When you speak your vocal cords shake the air around and make sound waves

Getting back to the analogy of Gravitational Waves

Above described circumstances in jungle is very much similar to what we study in the field of gravitational waves. Universe is the jungle, and Earth is your helicopter in this case. You can look at the sky and are able to see some celestial objects like planets, stars, comets and etc with naked eye or even with modern telescopes. They are the birds above the trees that we can see them but can’t hear them. But this is not everything which exists in the jungle. There are some animals hidden by trees that there is no way to see them even with modern telescopes [Gravitational Wave Sources]. The only way to detect them is listening to their voices [Gravitational Wave Signals]; however they are extremely weak compared to helicopter noise [Detector Noise]. You need to use your super-duper high-tech artificial ears [Gravitational Wave’s Detectors] to get some data, which is basically background noise plus some signal. People use Matched Filtering methods to filter out the signal from data. Post-Newtonian theory, for example, is your knowledge about the voice of a typical lion and if you want to know exactly the model of African lion voice you should use Numerical Relativity.


Universe as a jungle

Celestial objects as jungle animals including birds: stars, supernovas, galaxies, and lions [can’t see but can hear]: black holes and neutron star binaries

We actually use Post-Newtonian formalism to study the sound of a particular source: two angry lions fighting! [compact binary systems, e.g. two extremely massive black holes orbiting each other]. This is the most promising source of gravitational waves that ground current detectors on the earth can detect. One of our motivations to study this system is to find out if Mr. Einstein was right [2]. Gravitational wave astronomy will open a new window to the universe. In addition to the animals that we expect to detect their voices, some strange creatures, might be heard by this new generation of astronomy that we never expect. Somebody may has been “LOST” in spacetime from many years ago. Who knows?

We might hear voice of strange creatures (like super-massive BHs) in the jungle (universe) that we have never been aware of them before Gravitational Waves Astronomy

A good source: two angry lions fighting! [compact binaries]

Imagine in 3014, when kids will be learning Quantum Mechanics at kindergartens, they will learn the sounds of cosmic creatures at elementary schools. Latest modelings show that the voice of some sky animals are expected to be as followings.



  • Tigers: Equal mass binary gravitational waves: Two black holes, each of 50 solar masses [Listen
  • Lions: Extreme mass ratio binary gravitational waves: Initially circular orbit, into rapidly spinning BHs [Listen
  • Elephants: Extreme mass ratio binary gravitational waves: Initially circular orbit, into slowly spinning BHs [Listen
  • Monkeys: Extreme mass ratio binary : Initially highly eccentric orbit, into rapidly spinning BH [Listen]

  • Next generation of astronomers will “listen” to the sky instead of looking. Photo: My imaginary son which is an old fashion astronomer at right, and his son which is a modern astronomer at left, looking and listening to the sky from MIR-III space station. ©Photo by: my lovely great-granddaughter, who is not an astronomer but a poet.

    References

    [1] The title is borrowed from a Bernard Shutz's talk, "Gravitational Waves: Listening to the Music of the Spheres", public talk at Washington University in St. Louis, 2010.
    [2] Title of a book by C.M. Will, “Was Einstein Right?”, 2nd Edition, Basic Books, New York, 1993.

    Tuesday, March 18, 2014

    How to describe today's discovery to your grandma!

    BICEP2 telescope in South Pole
    Figure.1: BICEP2 telescope at South Pole
    Today, a major discovery in astrophysics has been announced by a research collaboration named BICEP2 which raised lots of interest, attention, and discussions in the science community as well as in public. Paolo already wrote a great note on this at The Gravity Room but here I would like to add another note to show you how I summarize the whole story to my grandma (or whoever else not in the field):
    1. Question: What they have discovered?
    Answer: A strong evidence for the existence of gravitational waves (GWs) coming all the way from the very early stages of the universe i.e. just after Big Bang explosion!
    More details: Using a modern telescope located at south pole, they have found another strong evidence for existence of GWs by studying the polarization of CMB (Cosmic Microwave Background) data. This is another indirect detection of GWs but not the first one. The first (indirect) detection was made by Hulse and Taylor (Nobel Prize winners of 1993) from a binary pulsar source while this recent experiment has detected the signature of GWs from the very early stages of the universe i.e. just after the Big Bang. Compared to the Hulse-Tayor's Binary Pulsar, in this case GWs are coming from completely different sources! Remember, we have not detected GW directly yet. This is what LIGO/VIRGO and other interferometric GW detectors are supposed to do in the next few years: the first direct detection of GWs...

    plot1
    Figure.2: Look grandma! This diagram is the heart of the story which compares the previous results (red) to BICEP2 results (blue) on measuring two parameters of CMBpolarization (vertical and horizontal axises). In another word, the red and blue areas show the allowed values of CMB polarization parameters based on the old and new experiments. New results (blue) clearly exclude the possibility of parameter "r" to be zero! This means a smoking gun for GWs coming all the way from Big Bang!
    2. Question: Why is it important?
    Answer: This is the first time that we have observed the signature of GWs from the Big Bang! It's quite exciting, isn't it? It also supports our early scenarios of the early universe and quantum gravity specially the Big Bang and Cosmic Inflation... In addition, if the results get confirmed by future experiments and the result holds up, it gives us an unprecedented view of the earliest moments in the history of the universe.
    3. Question: Should we celebrate now?
    Answer: Yes, but not too much! Because (1) Looking at the same thing (polarization of CMB in B-modes), soon, several similar experiments will come out with new data/results. So it's better to wait a bit and see the confirmations/disconfirmations... This is how science works! (2) A much bigger party is on the way: LIGO! In which we will be able to directly detect GWs from compact binary systems for the first time. LIGO will not only directly detect GWs but also will open a completely new branch of astronomy i.e. GW Astronomy; in which we can measure the physical parameters of the astronomical objects like sky-position, mass, spin, etc that for some cases we might not even be able to measure by other instruments such as optical-, radio-, x-ray-, and gamma-ray-telescopes.

    Figure.3: The frequency spectrum of Gravitational Waves and the sensitive range of different detectors. So, grandma! Focus on the "red" lines/notes. Looking at this figure, this is all they are talking about: using "Cosmic CMB polarization" as a detector to detect those GWs emitted from "quantum fluctuations in early universe" in the low frequency band of the spectrum. Notice that the primordial GWs coming from the early universe can be seen in a broad range of frequencies but CMB polarization experiments can only detect a small range of lower frequencies. Now you may ask "what do you need LIGO for while BICEP2 has already detected GWs!" Grandma! Look! Now focus on purple lines/notes and notice that the GWs that LIGO (one among other Terrestrial Interferometers) is supposed to detect is in the other side of the frequency spectrum for higher frequencies and for different sources including quantum fluctuations of early universe at much higher frequencies plus others sources such as compact binary systems and supernova explosions.
    Grandma! You should fight against gravity and stay tuned until the first detection announcement of LIGO in the next few years... Then we can totally celebrate testing the last untested piece of Einstein's General Theory of Relativity: Gravitational Waves!

    Saturday, January 4, 2014

    Back to Mississippi

    First time I went to Oxford Mississippi was 7 years ago, as a visiting master student at The University of Mississippi or, as it is more commonly known, OleMiss. I arrived there around May and, as in most college towns like Oxford, the city emptied right after the term finished, few days after my arrival. This is to say, nothing much was going on in Oxford at that time; nonetheless during my six-month visit there I managed to meet very interesting people, live curious experiences, have fun, and specially work hard in what has later become my field of research. Looking back, I had really a great time.

    This is why i'm so excited to come back in Oxford MS tomorrow to attend the Workshop "Testing General Relativity with Astrophysical Observations".

    The beautiful logo of the workshop recalls the iconographic Southern magnolia with the trajectory of an extreme mass-ratio inspiral, i.e. the evolution of a stellar-mass compact object orbiting a supermassive black hole like the one at the center of the Milky Way. [credits: Ana Sousa]

    This workshop will bring together experts in tests of general relativity, modified theories of gravity and astrophysics. The aim is to foster informal discussions on the current status of experimental constraints on Einstein’s theory and their prospects for the near future, when advanced gravitational-wave observatories will be operational.

    The list of participants is impressive and the program promises this will be a fun and fruitful meeting. For me this will also be a special experience, as at Olemiss I met some of my scientific advisors, some closest collaborators and also good friends.

    Oxford has been named by USA Today as one of the top six college towns in the U.S. and it is also known as the hometown of  Nobel-prize winning author William Faulkner, as well as residence of novelist and politician John Grisham. However, as a 23-yr old student, I like to remember myself walking around the Olemiss campus while listening to Afroman's hits, which are definitely less literate but undeniably fun. Here is an example, particularly apt for this occasion:




    OK, the lyrics is bitter and somehow sexist but, hell, Mississippi is not only Oxford!

    I better stop here and continue preparing my slides for this meeting....

    Thursday, December 26, 2013

    Measuring a black hole mass - you're doing it right



    1.  The orbit of every planet is an ellipse with the Sun at one of the two foci.
    2. A line joining a planet and the Sun sweeps out equal areas during equal intervals of time.
    3. The square of the orbital period of a planet is proportional to the cube of the semi-major axis of its orbit.
    Kepler's laws are among the most fundamental laws of astronomy.
    Basically, they describe the orbits of planets around the Sun (or any "small" object around a much more massive central object), under the assumption that the gravitational field can be considered Newtonian (even if historically quite the opposite happened, with Newton using Kepler's orbits to derive his laws of gravity).
    The orbits of all planets in the Solar system are very well described, to first order, by these laws. Only after centuries of observations of Mercury, the closest to the Sun, it was possible to notice post-Keplerian deviations due to relativistic effects.
    When Kepler's laws say "proportional", the proportionality factor involves the masses of the objects (this was found by Newton). For example, in this approximation the third law is actually
    where a is the semi-major axis of the orbit (the radius if the orbit is circular), G (=6.67384 × 10-11 m3 kg-1 s-2) the gravitational constant, M the mass of the central object, and T the orbital period.
    It is therefore possible to use the orbit of the small object to infer the mass of the big one, if we have an idea of the size of the orbit.

    One nice example? The measurement of our Galaxy's central supermassive black hole.
    Several groups have been able to measure accurately the mass of this black hole by tracking the movement of several stars around it.
    In the animated GIF above, a nice illustration of the procedure. Every orbit is an ellipse having in one of its foci, marked by the red cross in the center of the picture, an "invisible" object. This object, in order to describe the orbits of all the tracked orbiting points, must have a mass of about 4 million solar masses.
    Here is a quite complete description of the work done by several groups to obtain this result. 
    Enjoy!



    Friday, December 20, 2013

    Medium-sized black holes? Probably not.

    Ultraluminous X-ray sources (ULXs) are accreting black holes, i.e. black holes that are "eating" matter from a companion star. They are called ultraluminous because their luminosity is too high to be explained by "normal" accretion on stellar-mass black holes, i.e. black holes formed by the collapse of a single big star (from 8 up to ~100 masses of the Sun).
    A step behind. During accretion, matter falls towards a central object. This matter heats up in the process, and this heat is freed in form of radiation. This radiation in turn "pushes" on the matter that keeps falling in, and a point is reached when the luminosity produced is comparable to the push by the infalling matter and so no higher luminosity can be achieved. This is called the Eddington luminosity and is a well known quantity in accretion studies. This luminosity scales with the mass of the central object, so that supermassive black holes (billions of times the mass of the Sun) will be able to radiate at much larger luminosities than stellar-mass black holes (mass several times the Sun)
    Well, ULXs radiate at much more than the Eddington luminosity for stellar-mass black holes, so the first things that comes to mind is that they are bigger than stellar-mass black holes, and so they are members of the evasive class of Intermediate-mass black holes. Right?
    Not so fast, my friend. People like these japanese researchers have done a great deal of simulations to show that it is possible to overcome the Eddington limit some extent.
    Only problem: it was impossible to tell which of the two hypotheses was more right until 2012, since the few X-ray satellites capable of observing ULXs were sensitive only up to 10 keV, where the models started to really give incompatible predictions.
    In this old post we talked about the launch of the NuSTAR satellite. Well, that was the turning point.
    NuSTAR observed several ULXs and was able to finally strongly point in one direction. See the animated GIF above: the blue points are NuSTAR data, and they clearly follow better two models (the ones cutting off above 10 keV) than the others, while data from the XMM satellite weren't able to make a difference. This cutoff is considered a signature of super-Eddington accretion and permitted to estimate the mass of these ULXs to be in the high-end of the stellar-mass range.

    Here is a press release of these studies. Enjoy!

    Sunday, December 15, 2013

    Enrico Fermi on Einstein's theory of special relativity

    Yesterday I came across some fantastic notes by a young Enrico Fermi on Einstein's special relativity, which were included in "Asimmetrie", an outreach magazine issued by the Italian Institute for Nuclear Physics (INFN). After some search I found an English translation (by Robert Jantzen, I think).

    The reading is really mind-blowing (well, at least for me...) and even more so considering Fermi was 21 at the time...

    Enjoy!

    Apparently, there are no pictures of Fermi and Einstein together, so I turned down to this one...















    Wednesday, December 11, 2013

    Recommended by us: "MicroBooNE, in 3-D"

    Tingjun Yang (left) and Wesley Ketchum lead the effort to develop new 3-D reconstruction 
    software for the MicroBooNE experiment. Here they stand inside the MicroBooNE 
    time projection chamber.Photo: Reidar Hahn

    “ 
    Imagine your job is to analyze the data coming from Fermilab's MicroBooNE experiment. 

    It wouldn't be an easy task. MicroBooNE has been designed specifically to follow up on the MiniBooNE experiment, which may have seen hints of a fourth type of neutrino, one that does not interact with matter in the same way as the three types we know about. The big clue to the possible existence of these particles is low-energy electrons.
    But that experiment could not adequately separate the production of electrons from the production of photons, which would not indicate a new particle. MicroBooNE's detector, an 89-ton active volume liquid-argon time projection chamber, will be able to. To take advantage of this, every neutrino interaction in the chamber will have to be examined to determine if it created an electron or a photon.
    And there will be a lot of interactions to study — the MicroBooNE collaboration expects to see activity in their detector once every 20 seconds, including nearly 150 neutrino interactions each day.
    If all goes to plan, human operators won't have to worry about any of that. When MicroBooNE switches on next summer, it will sport one of the most sophisticated 3-D reconstruction software programs ever designed for a neutrino experiment.
    According to Wesley Ketchum and Tingjun Yang, two postdocs leading the software development team at Fermilab, MicroBooNE's computers will be able to accurately reconstruct neutrino interactions and automatically filter the ones that create electrons. The key to accomplishing this lies in the design of the time projection chamber.


    Continue to read on Fermilab Today